adsabs/AstroCLIMB huggingface dataset:
Paper: Hybrid Emission Modeling of GRB 221009A: Shedding Light on TeV Emission Origins in Long GRBs
Authors: Hebzibha Isravel, Damien Bégué, Asaf Pe'er
Figure caption: Left: the spectral energy distributions (SEDs) for p  e  = 8/3 and p  p  = 23/10 at different times, t = 235 s (dashed) and t = 4000 s (solid). The parameters are E 54 = 50, n 0 = 50, ϵ  p,−1 = 8, and ξ  p  = 0.04, leading to ϵ  B  = 0.186, ϵ  e  = 0.0014, ξ  e  = 0.01, and α = 6. Right: the SEDs for p  e  = 8/3 and p  p  = 22/10, the other parameters are E 54 = 30, n 0 = 30, ϵ  p,−1 = 8, and ξ  p  = 0.1, corresponding to ϵ  B  = 0.17, ϵ  e  = 0.002, ξ  e  = 0.01, and α = 6. The blue line represents the electron-synchrotron component, the red line represents the proton-synchrotron emission, and the black line specifies the IC component.
Paper: Hybrid Emission Modeling of GRB 221009A: Shedding Light on TeV Emission Origins in Long GRBs
Authors: Hebzibha Isravel, Damien Bégué, Asaf Pe'er
Figure caption: The parameter regime ϵ  B , ϵ  e , and ϵ  p  is explored in the context of p  e  = 8/3, p  p  = 23/10, E 54 = 50, and n 0 = 50, corresponding to ξ  e  = 0.01 and ξ  p  = 0.04 for the condition of Equation (25). Notably, the proton-synchrotron process dominates mostly in regions where ϵ  B  > ϵ  e  (Zone (ii)), while the SSC process takes over when ϵ  e  > ϵ  B  (Zone (i)). Zone (ii) is shown to have different boundaries based on the value of ϵ  p , and these boundaries visually distinguish both the regions. It is clear that the dominance of proton-synchrotron emission becomes more prominent as ϵ  p  increases. The hatched regions represent the condition ϵ  B  + ϵ  p  + ϵ  e  ≤ 1 for each ϵ  p  value and are regarded as forbidden zones.
Paper: Hybrid Emission Modeling of GRB 221009A: Shedding Light on TeV Emission Origins in Long GRBs
Authors: Hebzibha Isravel, Damien Bégué, Asaf Pe'er
Figure caption: Parameters ϵ  B  (top) and ξ  e  (middle) as functions of the total energy and ambient density, E 54 and n 0, for ϵ  p  = 0.8 where an assumed fraction of 10% of the protons are accelerated into a power law (ξ  p  = 0.1, left) and 1% are accelerated into a power law (ξ  p  = 0.01, right). Bottom: the acceleration efficiency, α as a function of E 54 and n 0. The plots are obtained from Equations (19), (23), and (20), respectively. The white region is forbidden, as it corresponds to ϵ  B  > 1 as seen from the top panel. The assumptions p  e  = 8/3 and p  p  = 2.3 are enforced for these figures.
Paper: Hybrid Emission Modeling of GRB 221009A: Shedding Light on TeV Emission Origins in Long GRBs
Authors: Hebzibha Isravel, Damien Bégué, Asaf Pe'er
Figure caption: The multiwavelength afterglow light curve for the proton-synchrotron model along with the observed data of GRB 221009A for p  e  = 8/3, p  p  = 23/10, E 54 = 50, n 0 = 50, ϵ  p,−1 = 8, and ξ  p  = 0.04, corresponding to ϵ  B,0 = 0.186, ϵ  e,0 = 0.0014, and ξ  e  = 0.01. The Swift-UVOT (white filter) and BAT data were retrieved from Tables 4 and 6 of Williams et al. (2023), and the Fermi-LAT data were obtained from Table 5 of Laskar et al. (2023b). The optical data is corrected for galactic extinction with A v = 5.4 (Fulton et al. 2023; Shrestha et al. 2023). The black dotted line at 226 s marks the onset of the afterglow phase corresponding to LHAASO-Collaboration et al. (2023), while the black dashed line at T 0 = 597 s marks the afterglow onset determined by Lesage et al. (2023).
Paper: Carbon Stars as Standard Candles: An Empirical Test for the Reddening, Metallicity, and Age Sensitivity of the J-region Asymptotic Giant Branch (JAGB) Method
Authors: Abigail J. Lee
Figure caption: The difference between the injected and recovered magnitudes for the entire catalog of artificial stars in brick 21 field 15 from Williams et al. (2014). The measured median offsets in bins of 1 mag, shown as red points, were all less than 0.003 mag.
Paper: Predicting the Yields of z > 6.5 Quasar Surveys in the Era of Roman and Rubin
Authors: Wei Leong Tee, Xiaohui Fan, Feige Wang, Jinyi Yang, Sangeeta Malhotra, James E. Rhoads
Figure caption: Color–color diagram for the z = 6.5–7.5 quasar color selection. Detailed modeling and full color selections can be found in Sections 3.2 and 4.1. The red tracks are quasar model colors based on the simulation described in Section 4.1, red circles denote a redshift grid with Δz = 0.1 spacing. The blue squares denote median cosmoDC2 ETG colors with z = 1.0, 2.0 labeled, gray contours denote the entire galaxy population with 4 iso-proportions of densities from 0.2–0.8 (limited to J=25.5 since fainter galaxies are excluded as discussed in Section 5.1). The green stars represent the MLT model colors with M0, L0, and T0 labeled. We also show orange points of spectroscopically confirmed MLTs in Best et al. (2020). Left: zYJ colors for LSST and WFI. Quasars at z > 6.5 have their Lyα break gradually shifted into longer wavelength IR bands, leaving them almost undetectable flux in the z band, increasing their z − Y colors with redshifts. The majority of the non-quasar population have bluer colors on the vertical axis. Middle: YJH colors for LSST and WFI. At z > 8.5 Lyα break shifts from Y to J, resulting in redder Y − J colors. From the color tracks it is obvious that z > 8.0 quasars suffer less contamination from other populations. Right: JHF colors for LSST and WFI. Note that the late T population (T6 and later) generally have bluer JHF colors and are easily excluded using this color plot.
Paper: Predicting the Yields of z > 6.5 Quasar Surveys in the Era of Roman and Rubin
Authors: Wei Leong Tee, Xiaohui Fan, Feige Wang, Jinyi Yang, Sangeeta Malhotra, James E. Rhoads
Figure caption: Candidate population surface densities as a function of J band magnitude. Detailed models can be found in Section 3.2. The vast difference in quasar and galaxy densities in faint magnitudes points out the distinct target strategy between Barnett et al. (2021) (see Figure 3 in their work) and this work. Red dashed line: quasars, by extrapolating the LF and spatial density decline rate in Barnett et al. (2019), and integrating over redshift z = 6.5–9.0. Red solid line: quasars using parameters from Wang19 and Matsuoka18, integrated over redshift z = 6.5–9.0. Blue dashed line: COSMOS quiescent-flagged galaxies at redshift z = 1–2. Blue solid line: cosmoDC2 red sequence galaxies at redshift z = 1–2. Green dashed line: MLTs summed over all spectral types (M0-T8) modeled in Barnett et al. (2019). Green solid line: MLTs summed over all spectral types in this work (M0-T9) with a slight difference in early M population densities.
Paper: Predicting the Yields of z > 6.5 Quasar Surveys in the Era of Roman and Rubin
Authors: Wei Leong Tee, Xiaohui Fan, Feige Wang, Jinyi Yang, Sangeeta Malhotra, James E. Rhoads
Figure caption: Wavelength coverage and depth of each survey up for the full mission time span. Both Roman HLS and Rubin LSST will reach a 5σ depth of 26 in general. We do not use LSST NIR y band because it is shallower than the Y band with Roman WFI.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: The number of galaxies with redshifts detected by JWST (left) and the corresponding mean bias (right), as a function of JWST pointings, N p, observed for 100 hr (solid curves) and 30 hr (dashed curves) of total time. This includes 20 minutes of slew time and instrumental overhead for each field. We show results for our three methods of redshift detection: low-resolution Lyman-break (﹩{ \mathcal R }=30﹩), high-resolution Lyman-break (﹩{ \mathcal R }=200﹩), and Lyα line detection.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: The illustrative case of correlating JWST with an SVL IM survey (i.e., one where the instrumental noise is zero). Left panel: the S/N of the cross-power spectrum of IM survey and N g = 25 JWST pencil beans with 100 hr of total integration time as a function of k. We include both the S/N computed with our full Fisher matrix calculation (Equation (3)) and the analytic approximation in Equation (6). For most of the points plotted, they agree better than ∼1%. Right panel: the value of the cross-power spectrum and the associated error bars (computed with the Fisher matrix formalism). The units are arbitrary since the S/N does not depend on the overall normalization of the cross-power spectrum when there is zero detector noise. The nonuniform size of the error bars with wavenumber is due to variations in the number of modes that fall into a bandpower bin.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: S/N of the cross-power spectrum when only including one SVL IM Fourier mode and for different grid spacings covering a subset of the IM field. The mode is assumed to be perpendicular to the line of sight and different wavelengths given by λ = 2π/k ⊥ are explored, although the sensitivities for inclined modes are similar as long as the parallel wavenumber is less than k ⊥. The pencil-beam field survey consists of 25 fields arranged in a grid with uniform spacing that varies from compact to covering the entire IM survey (assuming 100 hr of JWST time and the high-resolution Lyman-break mode for redshift measurement). The sensitivity computation is completed with the full Fisher formula given in Equation (3). An S/N = 1 corresponds to the best that is possible due to sample variance. Large-wavelength modes are best measured by wide grid spacing, as one would expect.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: Impact of JWST field configuration on the error of the galaxy-IM cross-power spectrum. As in Figure 2, we consider 25 JWST fields distributed within our SVL IM survey with 100 hr of total JWST time. We consider three configurations: a “random” distribution, a lattice spread evenly across the IM survey, and a “tight” lattice with the fields adjacent to one another and only spanning (40 Mpc)2 of the (300 Mpc)2 IM survey (see diagram in right panel; note that the size of points in this diagram are not meant to match the 8 Mpc × 8 Mpc JWST FOV). We plot the ratio of the tight and grid errors with the random case (left panel). All calculations are done with the full Fisher matrix formalism in Equation (3).
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Normalized integrated profiles of XTE J1810−197 (MJD: 58501−59427) at 2.25 (red solid line) and 8.60 GHz (blue dotted line). The observing date (MJD) and length is labled on the top left and top right corner of each profile, respectively. The black solid border includes the integrated profile with IP on MJD 58552 and more detail can be seen in the third panel of Figure 2.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Example of emission state and evolution of ﹩\bar{m}﹩. Upper two panels: example of normal emission state on MJD 58502 and spiky emission state on MJD 59096. The top panel shows the normalized integrated profile (solid line), m  i  (solid line with error bars), and σ 2 (gray solid line with open circles) for 2.25 (red plots) and 8.60 GHz (blue plots). We also show the pulse stack in the bottom panel of these two subfigures. The unusually large spaces between some pulse profiles are caused by removed sub-integrations because of RFIs. Bottom panel: evolution of ﹩\bar{m}﹩.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Examples of 12 general types of integrated profiles and the component naming convention. The integrated profiles at 2.25/8.60 GHz are shown in each subfigure with the red solid line and the blue dotted line, respectively. Prominent components in the profile are labeled P1–P7 by the pulse phase and divided with vertical black dotted lines. The IP (P7) is magnified and represented in the third panel.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: Top panels:the total S/N for our SPHEREx Lyα IM and JWST pencil beam example as a function of the number of JWST fields, N  p , for fixed total observing time. The left panel is for the case where JWST galaxy redshifts are determined with the Lyman break (with ﹩{ \mathcal R }=30﹩), and the right panel is for the Lyα line. The solid (dotted) curves represent the S/N on the cross-power when cross-shot power is not (is) included. Bottom panels: the galaxy-Lyα cross-power spectrum with errors for the Lyman-break (left panel) and Lyα redshift measurement case (right panel). We show errors for 100 hr of JWST time and N p = 144 (N p = 169), which maximizes the S/N in the cross-power spectrum in the Lyman-break (Lyα) case. The solid curves represent the total cross-power spectra, while the dotted and dashed curves represent the clustering and shot components, respectively.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Top panel: the phase of the component’s peak. The peak position in phase is divided into six parts with the horizontal black dashed line. The typical types of integrated profiles are separated by the vertical black dotted line except Type 3. Type 3 is marked with a vertical green dotted line. All partitioning of component and profile types are consistent with Figure 2. Bottom panel: W 10 of the P1/2 radiation region.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: The total S/N (defined as the square root of the S/N in our k-bins added in quadrature) on the cross-power spectrum for galaxies detected with JWST and our SVL IM survey (computed with Equation (6)). We show the total S/N for 30 (blue curves) and 100 hr (green curves) of total JWST observation times varying the number of randomly positioned pencil beams, N p. Results are included for each of the three ways of measuring galaxy redshifts described in Section 3: ﹩{ \mathcal R }=200﹩ Lyman-break, ﹩{ \mathcal R }=30﹩ Lyman-break, and Lyα. The S/N is maximized for N p similar to that where the most galaxy redshifts are detected.
Paper: Cross Correlation of Pencil-beam Galaxy Surveys and Line-intensity Maps: An Application of the James Webb Space Telescope
Authors: Eli Visbal, Matthew McQuinn
Figure caption: The total S/N on the cross-power spectrum for our HERA-JWST cross correlation example with 200 JWST hours spread over N  p  pointings. The blue, green, and red curves are for 1×, 10×, and 100× the HERA nominal integration time, respectively. We note the total S/N in the auto 21 cm power spectrum in the single FOV of HERA considered is 2.4, 12, and 29 for 1×, 10×, and 100× the HERA nominal integration time, respectively.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Plots showing T obs, ν, ﹩\dot{\nu }﹩, S 2.25, S 8.60, and α changing with time. (a) The scales of red and blue colored bars represent the length of data at 2.25/8.60 GHz that are chosen to do timing analyses, respectively. (b) The black triangle markers and blue circle markers show the timing result using dual-frequency and single 8.60 GHz observing data, respectively. The best fit ﹩\dot{\nu }﹩ is shown with the black solid line. (c) Same marker scheme as the above panel. (d) Evolution of flux density. (e) These spectral indices obtained with the single power-law function.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Integrated profile on 120 minute timescales at the spiky emission state on MJD 59209. Top panel: normalized integrated profiles of 414.5 minutes integration time at 2.25 (red solid line) and 8.60 GHz (blue dotted line). Bottom panel: normalized integrated profiles on 120 minutes timescales (three integrated profile on the bottom) and on the 54.5 minutes timescales (top integrated profile).
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Evolution of emission height r at 2.25 (red solid line) and 8.60 GHz (blue dotted line) with twist of the magnetic field ρ.
Paper: Simultaneous 2.25/8.60 GHz Observations of the Magnetar XTE J1810-197
Authors: Zhi-Peng Huang, 志鹏 黄, Zhen Yan, 振 闫, Zhi-Qiang Shen, 志强 沈, Hao Tong, 号 仝, Jian-Ping Yuan, 建平 袁, Lin Lin, 琳 林, Rong-Bing Zhao, 融冰 赵, Ya-Jun Wu, 亚军 吴, Jie Liu, 杰 刘, Rui Wang, 睿 王, Xiao-Wei Wang, 啸威 王
Figure caption: Abrupt variation of XTE J1810−197 on MJD 59075: phase-time waterfall plot at 2.25 (left panel) and 8.60 GHz (right panel); integrated profile on first 144 minutes (green solid line) and final 2.5 minutes (red dashed line).
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The relation between H I-to-optical-disk size ratio (R H I /R 25,g ) and strengths of environmental effects in galaxies. The size of the symbols have the same meanings as those in Figure 4, and gas-rich and -poor galaxies are plotted as blue and pink circles, respectively. In panels (a) and (b), high-mass galaxies are hatched with gray lines and are not included in the linear fitting or correlation analysis. The typical uncertainties are given at the lower-left corner of each panel. (a) Size ratio plotted against tidal strength S tid. For low-mass gas-poor and -rich galaxies, the Spearman rank correlation r s and the p-value are given at the upper-right corner in respective colors, the uncertainties of which are obtained with bootstrap. The bisector linear fitting of the low-mass gas-poor sample is plotted as the dashed magenta line, with two orthogonal fittings as dotted lines. The bisector fitting line crosses the R H I  = R 25,g  line (dashed gray), at log S tid = −1.87 ± 0.51. The slope k of the line is also reported with the fitting uncertainty. (b) Size ratio plotted against RPS strength S RPS. Galaxies with the lowest 10% of S RPS’s are not used for correlation calculation or fitting, and they are covered in shading. The intercept of the bisector fitting line is log S RPS = −0.91 ± 0.55. Panels (c) and (d) are the same as (a) and (b), except that only the TS sample or the RPS sample is plotted, that high-mass galaxies are included, and that the gas-rich and gas-poor samples are not distinguished. The intercepts are −1.52 ± 0.27 and −0.34 ± 0.14, overlapping the 1σ confidence intervals of those in panels (a) and (b).
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The relation between RPS and tidal interaction among H I-detected galaxies. Circles represent individual galaxies, color-coded by the deviation from the mean M H I  relation. Their radii are proportional to the stellar mass. (a) Environmental strength S RPS vs. S tid. The Spearman rank correlation r s and the p-value are given at the lower-right corner, the uncertainties of which are obtained with bootstrap. The last 10% of S RPS’s are not included in correlation calculation and are covered with the gray shaded region. The line of S RPS = S tid is drawn as the dotted gray line. Five galaxies have so little H I gas that 1.5R H I  is smaller than R 25,g . As a result, its S RPS is infinite, and it is plotted as an arrow pointing rightward. The typical uncertainties of S tid and S RPS are given at the lower-left corner. (b) Strippable gas fraction f RPS vs. f tid. Only galaxies with both f nonzero are plotted. The line of f RPS = f tid is drawn. The correlation between f RPS and f tid is given. The typical uncertainties of f tid and f RPS are given at the lower-left corner (only one side of the error bar is plotted due to limited space).