adsabs/AstroCLIMB huggingface dataset:
Paper: Application of Deep Reinforcement Learning to Major Solar Flare Forecasting
Authors: Kangwoo Yi, Yong-Jae Moon, Hyun-Jin Jeong
Figure caption: Training curve tracking the average rewards of the 10 models based on Model 3, using the test data set. Each value is the average reward of the models per epoch.
Paper: Public Data Release of the FIRE-2 Cosmological Zoom-in Simulations of Galaxy Formation
Authors: Andrew Wetzel, Christopher C. Hayward, Robyn E. Sanderson, Xiangcheng Ma, Daniel Anglés-Alcázar, Robert Feldmann, T. K Chan, Kareem El-Badry, Coral Wheeler, Shea Garrison-Kimmel, Farnik Nikakhtar, Nondh Panithanpaisal, Arpit Arora, Alexander B. Gurvich, Jenna Samuel, Omid Sameie, Viraj Pandya, Zachary Hafen, Cameron Hummels, Sarah Loebman, Michael Boylan-Kolchin, James S. Bullock, Claude-André Faucher-Giguère, Dušan Kereš, Eliot Quataert, Philip F. Hopkins
Figure caption: Schematic diagram of FIRE-2 simulation data, showing the names of directories and files as available via FlatHUB at http://flathub.flatironinstitute.org/fire. This data release includes three suites of simulations, each within its own directory (top row in blue): the Core suite to z = 0, the Massive Halo suite to z = 1, and the High Redshift suite to z = 5. Each suite contains a directory for each simulation (second row in green). This diagram shows the contents of the m12i simulation from the Core suite as an example, where “NNN” represents each snapshot index and “*” represents a wild card in the file name. All suites and simulations have similar data structure, with minor variations; see Section 4 for details.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: The distributions of the accretion rates of radio galaxies. The red line shows FR II radio galaxies and the green line shows FR I radio galaxies.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relations between jet radiation power (top) and jet kinetic power (bottom), respectively, and accretion disk luminosity for radio galaxies. The red dots show FR II radio galaxies and the green dots show FR I radio galaxies. The solid lines correspond to the best-fitting linear models obtained with a symmetric least-squares fit. The dashed lines indicate 3σ confidence bands. ﹩\mathrm{log}{P}_{\mathrm{rad}}=(0.33\pm 0.17)\mathrm{log}{L}_{\mathrm{disk}}+(27.53\pm 7.07)﹩; ﹩\mathrm{log}{P}_{\mathrm{jet}}=(0.51\pm 0.18)\mathrm{log}{L}_{\mathrm{disk}}+(22.97\pm 7.42)﹩.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relation between the jet kinetic power extracted from the underlying ADAFs for the BZ and hybrid models and the black hole mass, respectively. The ﹩\dot{m}=0.01﹩ and α = 0.3 are adopted (Narayan & Yi 1995). The spin of the black hole j = 0.98 is adopted. The red dots show FR II radio galaxies and the black dots show FR I radio galaxies. The orange line is the BZ jet model, and the blue line is the hybrid model.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: The fraction of the total jet power transformed into radiation (top), relativistic electrons (middle), and Poynting flux (bottom). The red dots show FR II radio galaxies and the green dots show FR I radio galaxies.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: Relation between IC luminosity and synchrotron luminosity for radio galaxies. The red dots show FR II radio galaxies and the green dots show FR I radio galaxies. The solid line corresponds to the best-fitting linear model obtained with the symmetric least-squares fit. The dashed lines indicate 3σ confidence bands.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: The distributions of physical parameters. The jet kinetic power is P jet = P B + P e + P p. The red line is for FR II radio galaxies and the green line is for FR I radio galaxies.
Paper: General Physical Properties of Gamma-Ray-emitting Radio Galaxies
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Xiaoling Yu, 效龄 俞, Nan Ding, 楠 丁, Dingrong Xiong, 定荣 熊, Xiaotong Guo, 晓通 郭
Figure caption: An example of a broadband SED of NGC 2484, modeled by using a one-zone model.
Paper: Mitigating Radio Frequency Interference in CHIME/FRB Real-time Intensity Data
Authors: Masoud Rafiei-Ravandi, Kendrick M. Smith
Figure caption: CHIME/FRB L4 events over a 24 hr period on 2020 September 12–13 (Figure courtesy of the CHIME/FRB collaboration). Repeating and nonrepeating FRB candidates are marked by black circles and green diamonds, respectively. “Galactic” and “known” events mostly refer to the same set of nearby sources, such as pulsars in the Milky Way galaxy. “Ambiguous” events often require human intervention in order to be classified as Galactic or extragalactic sources. In this example, three “RFI” storms (gray points) appear at t 1 ≈ 16–18hr (9/12), t 2 ≈ 20–22hr (9/12), and t 3 ≈ 2–7hr (9/13). Top panel: observed DM up to 13000 pc cm−3. For some unknown reason, most RFI storms tend to appear at relatively high DMs. In addition, aircraft transits appear as vertical lines of gray points with DM ≲103 pc cm−3 at t ≈ 17–21 hr (9/12). Middle panel: S/N with a minimum 8.5σ threshold. Bottom panel: north–south sky location based on 256 rows of digitally formed beams (each row contains four east–west beams, which are not shown here). The instrument has nonzero sensitivity in its sidelobes, which can continuously detect, e.g., the bright pulsar PSR B0329+54 for a few hours (see the arc centered at beam ≈ 145 and t ≈ 12hr (9/13)).
Paper: Mitigating Radio Frequency Interference in CHIME/FRB Real-time Intensity Data
Authors: Masoud Rafiei-Ravandi, Kendrick M. Smith
Figure caption: CHIME/FRB L1 data for a single beam, containing a pulsar transit along with RFI. Top panel:raw intensity with persistent RFI between 600 and 650 MHz. The relatively low-intensity region centered at ∼750 MHz corresponds to the long-term evolution (LTE) band, which is usually active. Multiple scatterings of radio waves off the feed structure cause the systematic “ripple” effect with a period of ≈30 MHz across the bandwidth (CHIME Collaboration 2022). Black regions indicate missing data. Middle panel: detrended intensity, including the missing data and RFI mask (black regions) prior to the dedispersion transform (see Figure 2). Dispersed sweeps (∝ν −2) across the bandwidth, particularly visible in the 600–400 MHz range at ≈2.2 s intervals, are signals from a nearby pulsar. Bottom panel: dedispersion space of events, including the pulsar (green and yellow dots at DM ≲100 pc cm−3). The RFI event at (t ≈ 128.8 s, DM ≈6500 pc cm−3) has a low signal-to-noise ratio (7 ≤ S/N < 10) and is below the detection threshold.
Paper: Mitigating Radio Frequency Interference in CHIME/FRB Real-time Intensity Data
Authors: Masoud Rafiei-Ravandi, Kendrick M. Smith
Figure caption: CHIME/FRB L1 pipeline for processing frequency-channelized intensity data in real time. L1 mitigates RFI for 16 k frequency channels (N  ν  = 16 k) by constantly generating a downsampled mask through a long sequence of operations inside the “subpipeline,” which reduces the overall computational cost by a factor ≈16 (see Figure 3). The RFI mask is upsampled back to 16 k frequency channels for detrending and dedispersing the raw intensity.
Paper: Mitigating Radio Frequency Interference in CHIME/FRB Real-time Intensity Data
Authors: Masoud Rafiei-Ravandi, Kendrick M. Smith
Figure caption: CHIME/FRB L1 data for three single beams, containing impulsive RFI that potentially triggers false positives in the downstream pipelines. Top row: raw intensity with persistent features as described in Figure 1. Black regions indicate missing data. Middle row: detrended intensity, including the missing data and RFI mask (black regions) prior to the dedispersion transform. Bottom row: dedispersion space of events, including residual-induced false positives (left and middle panels) and subthreshold (7 ≤ S/N < 10) high-DM false positives (right panel), which could result in, e.g., RFI storms (see Figure 5).
Paper: Mitigating Radio Frequency Interference in CHIME/FRB Real-time Intensity Data
Authors: Masoud Rafiei-Ravandi, Kendrick M. Smith
Figure caption: CHIME/FRB L1 subpipeline for generating dynamic RFI masks over intensity chunks with 1k frequency channels. Top panel: high-level diagram of the subpipeline, including the initial static mask, clipping and detrending transform chains in a specific order as described in Section 3. Middle panel: clipping transform chain that is iterated six times (circular arrow). Bottom panel: detrending transform chain, which is also executed for raw intensity data with 16 k frequency channels (see Figure 2).
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: Unbinned, unsmoothed Chandra merged image of 3C 297 in the energy band 0.3–7 keV. The three regions in which spectral analyses have been performed are highlighted in the blue regions (two circles and one ellipse). We detected 159 net counts in the extended emission region, 115 net counts in the nuclear region and 315 net counts in the hotspot region. The red dashed circle and ellipse mark the regions in which we observe an X-ray counts excess, due to the outflow (see Section 4.3 for more details).
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: Section of the GMOS preimage of the 3C 297 field. This i-band image has a total exposure time of 1080 s. Numbers correspond to the slit ID. The radio galaxy 3C 297 is close to the center of the image, identified with slit number 17. The bar on the lower left represents 30″. The different background levels are a due to limited processing functionality by the Gemini pipeline that automatically produces the preimage. North is up and east is left.
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: Example of the Gaussian decomposition applied to the observed emission line profiles. Left: fit to the coronal lines [Ne V] λλ3345, 3425. Right: [O II] λλ37286, 3729. For this latter line, a second blueshifted, broad component of FWHM = 1790 km s−1 was necessary to reproduce the observed profile. In both panels, the observed profile is in black, individual Gaussians are in blue, and the total fit is in red. The green line is the continuum level and the dashed maroon line is the residual after subtraction of the fit.
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: Top panel: Merged Chandra X-ray image (0.5–7 keV) showing the annuli used to extract surface-brightness profiles in four sectors. Blue ellipses represent the point sources excluded from each observation before merging the separate pointings. The source in the eastern region is unrelated. Bottom panels: Surface-brightness profiles for the regions highlighted in the top panel. In the western and eastern directions the emission cannot be fitted with a β-model.
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: New GMOS spectrum of 3C 297. The spectrum is displayed with a redshift correction of z = 1.408.
Paper: Powerful Yet Lonely: Is 3C 297 a High-redshift Fossil Group?
Authors: Valentina Missaglia, Juan P. Madrid, Mischa Schirmer, Francesco Massaro, Alberto Rodríguez-Ardila, Carlos J. Donzelli, Martell Valencia, Alessandro Paggi, Ralph P. Kraft, Chiara Stuardi, Belinda J. Wilkes
Figure caption: New GMOS spectra of targets in the 3C 297 field. All spectra are shown in the observed wavelength. The dashed vertical lines mark emission lines that were identified visually. Other apparently significant but unmarked lines are due to noise, which cannot be discerned from real lines at the resolution chosen for these plots.
Paper: Neutral Atmospheric Density Measurement Using Insight-HXMT Data by the Earth Occultation Technique
Authors: Wang-Chen Xue, Xiao-Bo Li, Shao-Lin Xiong, Yong Chen, Shuang-Nan Zhang, Li-Ming Song, Shu Zhang, Ming-Yu Ge, You-Li Tuo, Hai-Tao Li, Dao-Chun Yu, Dong-Ya Guo, Jia-Cong Liu, Yan-Qiu Zhang, Chao Zheng
Figure caption: The light curves observed by three X-ray telescopes of Insight-HXMT during a setting-type occultation of the Crab Nebula with a time bin of 0.5 s. The emission from the Crab Nebula is first occulted by the atmosphere and then by Earth. The dashed and dotted line indicates the time when the LOS altitude is 150 km and 40 km, respectively.
Paper: Neutral Atmospheric Density Measurement Using Insight-HXMT Data by the Earth Occultation Technique
Authors: Wang-Chen Xue, Xiao-Bo Li, Shao-Lin Xiong, Yong Chen, Shuang-Nan Zhang, Li-Ming Song, Shu Zhang, Ming-Yu Ge, You-Li Tuo, Hai-Tao Li, Dao-Chun Yu, Dong-Ya Guo, Jia-Cong Liu, Yan-Qiu Zhang, Chao Zheng
Figure caption: Earth occultation of the celestial source. The source appears to set (or rise) behind the limb of Earth, due to the satellite’s motion. The X-ray emission from the source will be occulted when the LOS pass through the atmosphere or Earth.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: EWs of H α  lines vs. stellar effective temperatures. Panels (a) and (b) are the results of dwarf stars, but for medium-resolution spectral (MRS) and low-resolution spectral (LRS) data, respectively. Panels (c) and (d) are results of giant stars, but for MRS and LRS data, respectively. Points in different colors represent different stellar types. Black dots are photospheric contributions of H α  lines calculated from the PHOENIX models. Dashed purple lines are baselines.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Comparison between Gaussian fitting and integration method for calculating the EWs of Hα lines. Panels (a) and (b) are the results of medium-resolution spectral (MRS) observations. Panels (c) and (d) are the results of low-resolution spectral (LRS) observations. Different colors represent different stellar types.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Examples of H α  emission lines of J034241.89+241158.3. The spectra are shifted for clarity.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Color–magnitude diagram. Sample of Wang et al. (2021) and our targets are shown in blue and red dots, respectively. Black star represents the Sun.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Comparisons of ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ derived from medium-resolution spectral (MRS) and low-resolution spectral (LRS) observations for different types of stars.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption:  χ vs. effective temperature. Blue dots and purple dots represent dwarfs and giants, respectively.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Histograms of stellar activity levels. Dwarfs and giants are denoted by blue and purple colors, respectively.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption:                       ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩–R o relations for medium-resolution spectral (MRS) and low-resolution spectral (LRS) observations. In panels (a) and (c) the relations are in linear-log scale while in panels (b) and (d) they are in log–log scale. Points with different colors represent different effective temperatures. Errors are shown in gray lines. Dashed magenta and black lines are the activity–rotation relations from Douglas et al. (2014) and Newton et al. (2017), respectively. Both the relations were shifted by Ro/3. Histograms along the R o axis are also presented.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Activity–rotation relations of different kinds of stars. From top to bottom corresponds to F-, G-, K-, and M-type stars. Panel (a) shows the results of medium-resolution spectral (MRS) data and panel (b) displays the results of low-resolution spectral (LRS) data. Again the dashed magenta and black lines are the shifted relation of Douglas et al. (2014) and Newton et al. (2017), respectively. Histograms along the ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ are also shown.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Plots of both phase folded light curves and ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ series.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Variability of the activity levels for different types of stars. The length of lines represent the variation ranges of ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ (upper panels) and ﹩{R}_{{\rm{H}}\alpha }^{+}﹩ (lower panels) for each target, based on their multiple observations.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Same as Figure 10 but for ﹩{R}_{{\rm{H}}\alpha }^{+}﹩.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Comparison of rotation periods derived in this work and in Reinhold & Hekker (2020).
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Same as Figure 9 but for ﹩{R}_{{\rm{H}}\alpha }^{+}﹩.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Same as Figure 4 but for an integration interval of 10 Å.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Comparison between ﹩{R}_{{\rm{H}}\alpha ,10\,\mathring{\rm{A}} }^{{\prime} }﹩ and ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩.
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Activity–rotations based on ﹩{R}_{{\rm{H}}\alpha ,10\,\mathring{\rm{A}} }^{{\prime} }﹩. Same as Figure 9, the plot is in linear-log scale in panel (a) and in log–log scale in panel (b).
Paper: Stellar Chromospheric Activities Revealed from the LAMOST-K2 Time-domain Survey
Authors: Henggeng Han, Song Wang, Yu Bai, Huiqin Yang, Xiangsong Fang, Jifeng Liu
Figure caption: Same as Figure 9 but for ﹩{R}_{{\rm{H}}\alpha ,10\,\mathring{\rm{A}} }^{+}﹩
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Hyperparameters obtained with the optimization procedure of Section 3.3. The black stars correspond to our best model, with all parameters optimized, while the green diamonds correspond to an additional model (used for robustness checks, see text for details) fixing the emission-line offsets α  j  = 0 ∀j and error floors γ  b  = 0.01 ∀b.
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Differences between the maximum a posteriori redshift estimates and the spectroscopic redshifts (divided by 1 + z) for the new model compared with the COSMOS2020 released LEPHARE and EAZY redshifts. This highlights the areas where they achieve similar performance in terms of scatter and outliers. Splitting between the three sources of spectroscopic redshifts also reveals the differences in photo-z performance for samples with different selection, as described in Section 4.
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Photo-z metrics calculated using our sample for our hierarchical model compared with the COSMOS2020 released LEPHARE and EAZY photo-z’s. We compute the median of ﹩{{\rm{\Delta }}}_{z}=({z}_{\mathrm{spec}}-{\hat{z}}^{\mathrm{MAP}})/(1+{z}_{\mathrm{spec}})﹩, as well as σ MAD = 1.48 × median(∣Δ z ∣), and the outlier fraction as the fraction of objects with ∣Δ z ∣ > 0.15.
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Maximum a posteriori redshift estimates versus spectroscopic redshifts for the three spectroscopic sources comprising the data we analyze. Differences are best highlighted in Figure 3, whereas these scatter plots with a logarithmic color bar better highlight the overall distributions and the outliers (which are rare).