adsabs/AstroCLIMB huggingface dataset:
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 stellar mass estimation. The quality of stellar mass estimation, in terms of σ NMAD, BIA, and OLF, is worse than that of redshift estimation and more sensitive to the selection of SED models. In the case with noise, for the most complicated SED model (SFH = α-β-τ-r, +CEH, DAL = Sal+18) used in this work, the σ NMAD, bias, and OLF of stellar mass estimation increase significantly when nlive > 100. This should be a clear indication of overfitting to the noise in the data. In general, more complicated SED models lead to worse quality of stellar mass estimation.
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: (a) Response functions for CSST and Euclid bands. (b) The modeled relation between magnitude and magnitude error for CSST bands. Sources with S/N < 1 (i.e., σ  m,i  > 1.08574) are considered as nondetections. The nondetections in a wavelength band i with an Nσ flux limit ﹩{F}_{\mathrm{lim},i}﹩ or magnitude limit ﹩{m}_{\mathrm{lim},i}﹩ are represented as sources with ﹩{F}_{i}={F}_{\mathrm{lim},i}﹩ and ﹩{\sigma }_{F,i}=-{F}_{\mathrm{lim},i}/N﹩ (the flux case) or with ﹩{m}_{i}={m}_{\mathrm{lim},i}﹩ and σ  m,i  = −1.08574/N (the magnitude case). These conventions make sure the conversion between flux data and magnitude data in the input file of BayeSED is consistent. (c)–(d) Same as (a) and (b), but for the COSMOS bands. For clarity, the 12 intermediate bands (IBs) and 2 narrow bands (NBs) are not shown.
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 joint distributions of the redshift and physical parameters of the empirical statistics–based mock galaxy population produced with BayeSED combined with SED models of different complexities. With the same set of empirical statistics, different SED models lead to slightly different redshift and age distributions, which is likely due to different mapping relations from the free parameters to the derived parameters. Meanwhile, only the two SED models with a quenching component produce a clear region of quiescent galaxies below the star-forming main sequence.
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 comparison of the redshift and magnitude distributions of the empirical statistics–based and Horizon-AGN hydrodynamical simulation–based mock galaxy samples.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: The neighborhood of Cygnus OB2. The ACIS-I mosaic of the Cygnus OB2 survey is outlined in black. Small circles indicate the massive OB star content of the region, regardless of spectral type and evolutionary class (Wright et al. 2015b). Diffuse X-ray contours corresponding to flux levels of (3.0, 3.7, 4.1, 4.7, 8.3) × 10−10 photons cm–2 s–1 arcsec–2 are shown in white. The false RGB color image was composed as follows: the Herschel 500 μm (T ≈ 10 K) cold gas emission in red, the 8 μm Spitzer IRAC image for the warm gas (T ≈ 150 K) in green, and the diffuse X-ray emission in the 0.5–2.5 keV energy range in blue. There are also four arrows that indicate the regions that show signs of the coexistence of 10 K cold ISM gas and hot diffuse X-rays, which are likely scenarios for CXE emission.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption:  Diffuse X-ray emission maps for ObsIDs 10939 to 10941: These observations are affected by the X-ray dust scattering halo produced by X-ray photons from the background source Cygnus X-3. The massive evolved binary system (O6IV + O9III) Schulte #3 shows a diffuse X-ray halo, with a typical HR ∼ 0.05–0.16. The single evolved stars WR 144, MT 138, and MT 140 do not show halo-like emission but appear to contribute to diffuse structures in the nearby regions through wind–ISM interactions (see discussion in Section 7). Maps for Obs IDs 10942 to 10944: Schulte #4 (O7III + ?) has an associated diffuse X-ray halo, even though it is a relatively faint X-ray point source (net counts 296 photons). In contrast, Schulte #20 (O9 III) does not produce a diffuse halo, although faint diffuse structures appear to be present (see HR maps), similar to the cases of the other evolved B-type massive stars (MT 191, 174, 108 and Schulte #2). Maps for ObsIDs 10945 to 10948: The diffuse contribution in the lower right corner of ObsID 10947 is the Cygnus X-3 X-ray binary dust scattering halo (see discussion in Section 4.2).
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: The Cygnus OB2 HR diffuse map in the soft (0.5–2.5 keV) and hard (2.5–7.0 keV) bands. Spatial regions of diffuse gas that correspond to HR values lower than −0.1 were discarded (see Section 4). Small black circles indicate the MS massive stars of the region. Names and labels in white indicate the evolved stars with more intense stellar winds (Wright et al. 2015b). Names are omitted for main-sequence O- and B-type stars that have less massive winds. The X-ray mosaic intensity is logarithmically scaled.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Left: the X-ray diffuse emission map for the full Cyg OB2 FOV in the 0.5–7.0 keV band. Right: contours in ﹩\mathrm{log}({f}_{\mathrm{unresolved}})﹩ indicating the intensity levels expected from the X-ray flux of unresolved stars.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Curves representing the expected relative contribution of synchrotron to IC loses to the diffuse X-ray emission. The black solid line corresponds to the ratio U  B=4μG/U ph accounting for the total contribution from all massive stars of the region with respect to the center of the diffuse emission. The gray region represents distances from the adopted center (R.A. = 20:33:00, decl. = 41:20:00), in which diffuse X-ray emission is not observed.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: The Cygnus OB2 diffuse emission map in the 0.5–7.0 keV band. The full band is coded in color so that soft (0.5–1.2 keV) emission appears in red and medium (1.2–2.5 keV) emission appears in green, while hard (2.5–7.0 keV) emission appears in blue. Small white circles indicate the massive stellar content of the region. Names and labels indicate the evolved stars with more intense stellar winds. Names are omitted for main-sequence O- and B-type stars that have less massive winds. The X-ray mosaic intensity is logarithmically scaled, and the region shown is approximately 1.3 × 1.3 deg, with north up and east to the left.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Sample of some tessellate spectra for region Nos. 1, 4, 8, 12, 15, and 18. Models that describe diffuse X-ray emission are indicated with red solid lines. The thinner colored lines represent the decomposition of the total emission into different models: supersoft (SS—orange), soft (S—green), moderate (M—magenta), and hard (H—blue). Note: black dashed lines correspond to the residual instrumental line at ∼2.1 keV from background stowed spectra, which has not be taken into account for the event/stowed background normalization (see 2.2 for discussion).
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Left: tessellated X-ray surface brightness of the Cygnus OB2 region. The achieved S/N is 60, and regions were computed to perform spatially resolved X-ray spectral fitting. Regions labeled with dashed lines were not taken into account owing to the influence of the background-scattered X-ray radiation from Cyg X-3 (see discussion in Section 4.2). Right: diffuse X-ray mosaic events used for spectral extraction.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Stacked diffuse X-ray spectrum for the Cygnus OB2 region. The total (0.5−7.0 keV) diffuse X-ray fitted model (thick red line) has an intrinsic L tot of 5.6 × 1034 erg s−1. The total emission is decomposed into different models: supersoft (SS—orange), soft (S—green), moderate (M—magenta), and hard (H—blue).
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 Bayesian evidence (BE), maximum likelihood (ML), and metrics of photometric redshift (red cross), stellar mass (blue square), and SFR (green circle) estimation from the Bayesian analysis of the hydrodynamical simulation–based mock galaxy sample for the COSMOS-like survey employing six SED models (0: SFH = τ, –CEH, DAL = Cal+18; 1: SFH = τ, +CEH, DAL = Cal+18; 2: SFH = τ, +CEH, DAL = Sal+18; 3: SFH = β-τ, +CEH, DAL = Sal+18; 4: SFH = β-τ-r, +CEH, DAL = Sal+18; 5: SFH = α-β-τ-r, +CEH, DAL = Sal+18) with increasing complexity in the forms of SFH and DAL, as well as for cases with (bottom panels) and without noise (top panels). In the case without noise, the simplest model “SFH = τ, –CEH, DAL = Cal+18” has the lowest Bayesian evidence of ﹩\mathrm{ln}(\mathrm{BE})=-1,710,604\pm 6811﹩. Meanwhile, the SED model “SFH = β-τ, +CEH, DAL = Sal+18,” which is neither the simplest nor the most complex model, has the largest Bayesian evidence of ﹩\mathrm{ln}(\mathrm{BE})=387,009\pm 7273﹩, and gives the highest-quality parameter estimates. As in the cases of the CSST-like and CSST+Euclid-like surveys, the model selection with the maximum likelihood (or equivalently the minimum χ 2) leads to similar results. In the case with noise, the simplest model “SFH = τ, –CEH, DAL = Cal+18” still has the lowest Bayesian evidence of ﹩\mathrm{ln}(\mathrm{BE})=99,881\pm 4881﹩. Meanwhile, the SED models “SFH = τ, +CEH, DAL = Sal+18” and “SFH = β-τ, +CEH, DAL = Sal+18” have the largest Bayesian evidences of ﹩\mathrm{ln}(\mathrm{BE})=131,578\pm 5115﹩ and ﹩\mathrm{ln}(\mathrm{BE})=130\text{,}766\pm 5064,﹩ which are comparable within error bars. Unlike the cases of the CSST-like and CSST+Euclid-like surveys, the model selection with the maximum likelihood (or equivalently the minimum χ 2) leads to similar results. The two models with the largest Bayesian evidence (or maximum likelihoods) also give the highest-quality parameter estimates. In general, in the cases with and without noise, much clearer results of model comparison are obtained. Meanwhile, in the more realistic case with noise, the more complicated SED models are more favored than in the cases of the CSST-like and CSST+Euclid-like survey. All of these are natural results of the much stronger discriminative power of the COSMOS-like survey compared to that of the CSST-like and CSST+Euclid-like surveys.
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 from the Bayesian analysis of the hydrodynamical simulation–based mock data for the COSMOS-like survey employing the two SED models with the largest Bayesian evidence. By comparing with the results for the CSST-like survey in Figure 12 and those for the CSST+Euclid-like survey in Figure 17, it becomes clear that the quality of photometric redshift estimation is significantly increased in both cases with and without noise. In both cases, the best two SED models give an identical quality of photometric redshift estimation. In the case without noise, the bias and OLF of photometric redshift estimation are almost zero while the σ NMAD is only 0.002. Since the errors from parameter degeneracy and SED model errors should be largely reduced, this suggests that the contribution of errors from the stochastic nature of the MultiNest sampling algorithm and other potential errors in the BayeSED code should be less than 0.002. In the more realistic case with noise, the outliers caused by the misidentification of Lyman and Balmer break features are largely resolved.
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 17, but for the SFR. (a), (c) The cases without noise. By comparing with the results for the CSST-like survey in the left panels of Figure 14, it becomes clear that the σ NMAD and OLF of photometric SFR estimation are largely reduced, although the bias is slightly increased. Besides, with the more complicated β-τ form of SFH, the quality of photometric SFR estimation is improved. (b), (d) The cases with noise. By comparing with the results for the CSST-like survey in the right panels of Figure 14, all of the σ NMAD, bias, and OLF of photometric SFR estimation slightly increase. This suggests that the inclusion of the J, H, and Y bands from Euclid is not very helpful for improving the photometric SFR estimation. Besides, with the additional consideration of metallicity evolution, the quality of photometric SFR estimation becomes slightly worse.
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 17, but for the stellar mass. By comparing with the results for the CSST-like survey in Figure 13, it becomes clear that the quality of photometric stellar mass estimation is significantly improved in both cases with and without noise. Apparently, the inclusion of the J, H, and Y bands from Euclid is crucial for a more accurate estimation of stellar mass. Besides, with the more complicated β-τ form of SFH, the quality of photometric stellar mass estimation is only slightly improved.
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 21, but for the SFR. By comparing with the results for the CSST+Euclid-like survey in Figure 18, it becomes clear that the quality of photometric SFR estimation is significantly improved in both cases with and without noise. Besides, the more complicated β-τ form of SFH makes the quality of photometric SFR estimation much better.
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 21, but for the stellar mass. By comparing with the results for the CSST+Euclid-like survey in Figure 18, it becomes clear that the quality of photometric stellar mass estimation is improved further in both cases with and without noise. Besides, the more complicated β-τ form of SFH makes the quality of photometric stellar mass estimation a little better.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Relative ion abundances and their changes with decreasing κ. The individual colors denote the values of κ. Violet stands for κ = 1.7, while red denotes κ = 2. A variety of ions are shown, from the transition-region Si IV and Fe VIII to the coronal Fe XII and Fe XVII.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Electron κ-distributions as a function of electron kinetic energy E, plotted for various values of κ and log(T [K]) = 6.6.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Examples of the behaviors of the suppression factors for dielectronic recombination for a selection of ions. Individual values of κ and log(N e [cm−3]) are indicated.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: The effect of multi-ionization on the Fe ionization equilibrium for a Maxwellian distribution (top) and κ-distributions with κ = 5, 2, and 1.7 (rows 2–4). Calculations for all distributions, including the Maxwellian, were based on the ionization cross sections of Hahn et al. (2017) and recombination rates from CHIANTI version 10.1.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Silicon relative ion abundances (ionization equilibrium) for a Maxwellian distribution (top) and κ-distributions with κ = 5, 2, and 1.7 (rows 2–4). The individual line styles correspond to different values of log(N e [cm−3]). The calculations for all distributions, including the Maxwellian, were based on the ionization cross sections of Hahn et al. (2017) and recombination rates from CHIANTI version 10.1. Note that the effect of EIMI was included.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Relative ion abundances of Si IV (top), Fe VIII (middle), and Fe X (bottom), where the effects of finite density on dielectronic recombination are shown for Maxwellian distributions (left) and κ-distributions with κ = 2 (right). The calculations for all distributions, including the Maxwellian, were based on the ionization cross sections of Hahn et al. (2017) and recombination rates from CHIANTI version 10.1.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: The same as Figure 7, but for iron.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Dielectronic recombination rate coefficients, where the effects of finite density on dielectronic recombination are shown for Maxwellian distributions (left) and κ-distributions with κ = 2 (right). Several ions are shown: Si V, i.e., recombination from Si V to Si IV (top), Fe VIII (middle), and Fe X (bottom).
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 from the Bayesian analysis of the hydrodynamical simulation–based mock data for the CSST-like imaging survey employing the two SED models with the largest Bayesian evidence. (a) By comparing with the results in Figure 8(c), it becomes clear that, with the additional consideration of metallicity evolution and the adoption of the DAL of Salim et al. (2018), the σ NMAD of photometric redshift estimation is obviously reduced, although the bias and OLF are slightly increased. Meanwhile, the systematic patterns in the former results are also largely reduced. (c) By additionally employing a more complicated β-τ form of SFH, the σ NMAD of photometric redshift estimation is only slightly reduced while the bias and OLF are exactly the same. (b), (d) In the case with noise, the best two models are quite similar in their quality of photometric redshift estimation. Besides, there are two clear branches of outliers caused by the misidentification of Lyman and Balmer break features.