adsabs/AstroCLIMB huggingface dataset:
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Left: this panel illustrates a comparison between the power spectrum S  i  of the true wave-front deviation and the estimated deviation. The line plots represent the averages across 100 distinct optical states used to perturb the telescope, simulating for each state corner out-of-focus images under different atmospheric instances, each characterized by an average seeing of 0.″8. The x-axis delineates the various ﹩{\tilde{u}}_{i}﹩ modes within the wave-front deviation basis, encompassing 76 modes derived from the extended ﹩\tilde{U}﹩ basis via SVD. Right: here, we display the cumulative sum of singular values. The red dot marks the juncture where the cumulative contribution attains 99%, highlighting the significant portion of the total contribution captured by a subset of the modes.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Progression of key performance indicators for OIC and PID controllers over multiple iterations, corresponding to a sequence of elevations from the LSST baseline survey. The top-left graph highlights the FWHM evolution for both controllers. Surrounding plots detail the evolution across various degrees of freedom, distinguishing PID corrections (in a deeper color) from OIC corrections (in a lighter color). The bottom-right graph focuses on the force actuator rms evolution for the M1M3 and M2 mirrors, providing insight into the dynamic adjustments by both control strategies.
Paper: The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Guillem Megias Homar, Steven M. Kahn, Joshua M. Meyers, John Franklin Crenshaw, Sandrine J. Thomas
Figure caption: Left: displays the effective response matrix, VV  T , truncated at the 25th characteristic mode for the unscaled sensitivity matrix. Right: shows the effective response matrix, ﹩{\rm{\Omega }}\tilde{V}{\tilde{V}}^{\top }{{\rm{\Omega }}}^{-1}﹩, truncated at the 25th characteristic mode for the sensitivity matrix after applying the scaling factor Ω. This side highlights how scaling influences the system’s response, favoring M2 modes and including rigid body motions.
Paper: Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Xu-Zhi Hu, Xiaoyu Hong, Wei Zhao, Liang Chen, Wei-Yang Wang, Linhui Wu
Figure caption: Distribution of fractional polarization (color) at 1.7 GHz for the observation on 2000 February 7 superimposed on the corresponding total intensity contours. Contours are 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128). The blue arrow indicates the jet direction at the parsec scale.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Spatially resolved stellar populations of the three galaxies with z spec. Left: the RGB images are the same as those shown in Figure 3, except that here we zoom in to the central 1.″3 × 1.″3 region. The middle and right panels show the SED fitting results from our fiducial PROSPECTOR model (Section 2.4). Middle: the normalized (i.e., ﹩{F}_{\nu }^{{\rm{F}}150{\rm{W}}}=1﹩) photometry and best-fit SEDs of individual structural components defined in Section 2.3. These include best-fit SEDs for (1) visually identified clumpy substructures, which are color-coded accordingly based on the colors used in the RGB images for individual apertures, (2) the smooth component (orange), and (3) integrated flux (black). The inset highlights the wavelength range around 2μm covered by NIRCam F150W, F182M, F200W, and F210M, and HST/WFC3 F160W filters. The magenta shaded region marks the rest-frame wavelength range between 3645 and 4100 Å, which contains key spectral features sensitive to stellar age, such as the Balmer jump and D4000 break (A.G. Bruzual 1983; M. L. Balogh et al. 1999). Right: reconstructed nonparametric SFHs of individual substructures. Each SFH is normalized with its peak SFR, i.e., normalized SFR(t) = SFR(t)/max(SFR(t)), to better show the difference in the shape of SFHs. In each subpanel, we overplot the best-fit nonparametric SFHs for the smooth component (orange) and integrated flux (black). For better illustration, here we only plot the best-fit SFHs with solid lines, while in Appendix C, we also plot the 1σ uncertainties.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: The scatter plot of the intrinsic stellar masses of clumpy substructures (y-axis) vs. the total stellar masses of their host galaxies (x-axis). The black solid line marks the prediction of Toomre mass ﹩{M}_{\mathrm{Toomre}}﹩, which represents the largest stellar mass that a clump can form through Toomre instability in an unstable, gaseous disk (see Section 3.3). The dashed and dotted lines mark 2 × and ﹩3\times {M}_{\mathrm{Toomre}}﹩, respectively. The upper-left gray shaded region marks the unphysical part where ﹩{{M}}_{C}^{{\rm{int}}}\gt {{M}}_{* }﹩. The symbols used for individual galaxies, as well as the corresponding color scheme used for individual clumpy substructures, are labeled on the right. For low-mass clumps whose stellar masses are already less than ﹩{M}_{\mathrm{Toomre}}﹩ before subtracting the contribution from the surrounding smooth component (Section 3.2), we plot the upper limits of their ﹩{{M}}_{C}^{{\rm{int}}}﹩. Similar to previous plots, the stellar cores, C1, are color-coded in red. The filled symbols with error bars show the ﹩{{M}}_{C}^{{\rm{int}}}﹩ estimated via the method of Section 3.2.1, while the hollow symbols with dashed edges show the ﹩{{M}}_{C}^{{\rm{int}}}﹩ estimated via a different method described in of Section 3.2.2. We find that the intrinsic stellar masses of C1 are significantly larger than ﹩{M}_{\mathrm{Toomre}}﹩ in all six galaxies, suggesting that C1 may not form through in situ fragmentation due to Toomre instability.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Similar to Figure 6, but for the three galaxies with z phot shown in Figure 4. Note that the C2 of JADES-JEMS-11059 is not covered by its segmentation map (the bottom row of Figure 4), but we still include it in the analysis because its photometric redshift is consistent with that of the central galaxy.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Morphological analysis for the individual substructures. Each substructure is modeled as a Sérsic profile using the code FORCEPHO that adopts an MCMC framework to perform PSF-convolved analysis in individual exposures to better estimate the parameter uncertainties (Section 3.2). The best-fit centroids of individual substructures are marked with the star symbols. The left three columns show the F210M cutout, best-fit model, and residual, respectively. The fourth column shows the residual χ map, which is defined as χ = (data − model)/error, from which we clearly see the smooth component surrounding the clumpy substructures. The last column shows the posterior corner plot of Sérsic index n vs. circularized effective (i.e., half-light) radius R  e .
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: The star-forming main sequence of 3 < z < 4.5 galaxies from JEMS. The stellar mass and SFR are derived from SED fitting with integrated flux. Each galaxy is color-coded using its best-fit photometric redshift. The green solid line shows the star-forming main sequence at z = 3.7 for M * > 108.5 M ☉ galaxies from P. Popesso et al. (2023). We extrapolate it to M * < 108.5 M ☉, and plot it as the green dashed line. The green shaded region marks the ±0.3 dex range. Also plotted as the magenta solid line is the star-forming main sequence at z = 2.7 for M * > 1010.2 M ☉ galaxies from J. Leja et al. (2022), who also used PROSPECTOR with a similar SED model of this work. Similarly, we also extrapolate it to M * < 1010.2 M ☉, and plot it as the magenta dashed line. The six galaxies presented in this work are marked with golden hexagons. They are below the star-forming main sequence by ≈0.2−0.7 dex.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Comparisons of the stellar-mass (top panel) and star formation rate (SFR; bottom panel) measures. The x-axis shows the measure using integrated flux, and the y-axis shows the results by coadding the measures of individual structural components (i.e., substructures+smooth) together. We plot all 37 galaxies showing distinct substructures around the rest-frame 4000 Å (Section 2.1), and the final sample of six galaxies presented in this paper are marked with the red star symbols. We see excellent agreement between the two measurements.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: The stellar-mass surface density at the location of C1. The symbol used for each galaxy is the same as in Figure 9. The solid line shows the Σ1 kpc evolution of galaxies at 0.5 < z < 3 measured by G. Barro et al. (2017). We extrapolate this evolution to z > 3 and plot it as the dashed line. The evolution of star-forming galaxies and quiescent galaxies is plotted in cyan and magenta, respectively. The shaded region marks the ±0.3 dex range. Although the six galaxies have not quenched yet, their stellar-mass densities within the region of C1 are already high, approaching the central stellar-mass surface density of high-redshift quiescent galaxies (see Section 4.2 for detailed discussions and caveats of this comparison).
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: Comparisons among three different PSF models (Appendix A) for the NIRCam filters used by JADES. Plotted in the bottom of each panel are the differences between mPSFs and ePSFs (red dashed line), and between simple WEBBPSF models and ePSFs (blue dashed line), where the horizontal, gray dashed lines mark ±1% range. Excellent agreement is observed between ePSFs and mPSFs, while simple WEBBPSF models significantly deviate from ePSFs at small angular scales.
Paper: JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5
Authors: Zhiyuan Ji, Christina C. Williams, Sandro Tacchella, Katherine A. Suess, William M. Baker, Stacey Alberts, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Fengwu Sun, Daniel J. Eisenstein, Marcia Rieke, Michael V. Maseda, Kevin Hainline, Ryan Hausen, George Rieke, Christopher N. A. Willmer, Eiichi Egami, Irene Shivaei, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Tobias J. Looser, Roberto Maiolino, Chris Willott, Zuyi Chen, Jakob M. Helton, Jianwei Lyu, Erica Nelson, Rachana Bhatawdekar, Kristan Boyett, Lester Sandles
Figure caption: JADES PSF mosaics of NIRCam/F090W (left), F200W (middle), and F444W (right) filters produced following the procedure described in Appendix A.
Paper: A Deeper Look into eFEDS AGN Candidates in Dwarf Galaxies with Chandra
Authors: Adonis A. Sanchez, Amy E. Reines, Ákos Bogdán, Ralph P. Kraft
Figure caption: Left: three-color images of our target galaxies retrieved from the Dark Energy Camera Legacy Survey (DECaLS; A. Dey et al. 2019) with the z, r, and g bands depicting red, green, and blue, respectively. Right: Chandra X-ray images of the galaxies in the 0.5–7 keV band. We show the positions and the corrected combined positional uncertainty (based on the RADEC_ERR_CORR parameter from the eFEDS main catalog) in magenta. We also overlay the positions of our detected X-ray sources as red crosses. The green circles represent the ∼2″ apertures around the sources. The red circle shows the 95% positional uncertainties of the eROSITA-detected X-ray sources. Each Chandra-detected source falls within the positional uncertainty reported in the eFEDS main catalog, except for ID 1, which does not have a detectable X-ray source in the Chandra image.
Paper: A Deeper Look into eFEDS AGN Candidates in Dwarf Galaxies with Chandra
Authors: Adonis A. Sanchez, Amy E. Reines, Ákos Bogdán, Ralph P. Kraft
Figure caption: Hardness ratio vs. 2–10 keV band X-ray luminosity for our two galaxies with a detected X-ray source in at least one of the two bands. The hardness ratio was calculated using BEHR (see Section 4.1). The error bars are the 68% confidence intervals. Hardness ratios for unabsorbed power-law models with Γ = 1.8, 2.0, and 2.5 are depicted as solid gray lines, while the absorbed power laws with Γ = 1.8 are shown with gray dashed lines.
Paper: A Deeper Look into eFEDS AGN Candidates in Dwarf Galaxies with Chandra
Authors: Adonis A. Sanchez, Amy E. Reines, Ákos Bogdán, Ralph P. Kraft
Figure caption: X-ray energy spectra for the X-ray source detected in galaxy ID 2 (left panel) and for source X1 in ID 3 (right panel). The spectra were fit with absorbed power-law models, resulting in best-fit values of ﹩{\rm{\Gamma }}\,=\,{2.37}_{-0.32}^{+0.33}﹩ and ﹩{\rm{\Gamma }}\,=\,{1.66}_{-0.19}^{+0.25}﹩ for the sources in ID 2 and ID 3, respectively.
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: The initial parameter spaces for SNe Ia from Population III stars. Black filled circles represent the progenitor binaries of SNe Ia. Green triangles indicate systems that experience nova explosions, and the mass transfer rate is lower than the WD critical accretion rate. Open circles indicate that the mass transfer rate exceeds the WD critical accretion rate and the CE is formed, but the resulting CE is not massive enough that the WD cannot grow its mass to 1.378 M ⊙. The red crosses show the systems that experience dynamically unstable mass transfer, and the black crosses in the lower left are for donors initially filling their Roche lobe. The red solid lines and dashed lines show the boundaries for models that start mass transfer at the termination of central H burning and at the onset of He core burning, respectively. The initial WD masses are shown in the upper right of each panel.
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Panel (a): single and binary evolutionary tracks of Population III stars. The solid black lines represent evolutionary tracks of single stars with masses of 1.6, 2.4, and 3.6 M ⊙ from the bottom to the top, respectively. Thick blue, yellow, and green lines represent the evolutionary stages of central H burning, H-shell burning, and He-shell burning, respectively. Three typical tracks of donor stars in binary systems are shown in red lines from bottom to top, respectively. The onsets of mass transfer are shown in red squares, and the onsets of SN explosions are shown in red stars. The gray dashed lines represent lines of constant radius. Panel (b): the accretion processes of WDs during the mass transfer stages for the binary with initial parameters of M d,i = 1.6 M ⊙, M WD,i = 1.1 M ⊙, and Pi = 0.38 days. The accretion rate of the WD and the mass transfer rate are shown in red solid lines and black dashed lines. The stable burning regions are shown in the red shaded region. Panel (c): similar to panel (b) but for a binary with initial parameters of M d,i = 2.2 M ⊙, M WD,i = 1.1 M ⊙, and Pi = 8.4 M ⊙. The mass of the CE, M CE, is shown in a blue dashed line. This binary system does not eventually result in an SN explosion, and the WD mass at the termination of mass transfer is 1.32 M ⊙. Panel (d): similar to panel (c) but for a binary with initial parameters of M d,i = 3.6 M ⊙, M WD,i = 1.1 M ⊙, and Pi = 37.0 M ⊙.
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Upper panel: the birthrate of SNe Ia as a function of redshift. The total birthrate of SNe Ia from Population III stars of the S19 model is shown in a blue solid line, and the contributions of the SD and DD channels are shown in blue dashed and dotted lines, respectively. The observed SN Ia rates at z < 2 are shown in gray dots with error bars (collected by Strolger et al. 2020). The black solid line is the best-fit curve obtained with the convolution of the Population I/II CSFH and a power-law DTD from Maoz & Graur (2017). We make a cutoff for Population I/II SN Ia rates at z = 6. The simulated SN Ia rate with theoretical DTDs of Population I stars is shown in the red solid line, where the contributions of the SD and DD channels are shown in red dashed and dotted lines, respectively. The observed rates are about twice as high as the rates from theoretical simulations mainly because the DTD in the observations is generally larger than the theoretical simulations. The corresponding cosmic time is shown on the upper axis. See more details in the text. Lower panel: the scaled SN Ia rate as a function of redshift. To match the observations, we artificially scale up the SN Ia rates by a factor (2.2), so that the fitted and theoretical curves of Population I/II SN Ia rates have the same value at z = 0.
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Upper panel: the evolutionary tracks of stars with masses from 3.6 to 9.0 M ⊙ in steps of 0.2 M ⊙. The cyan lines represent the stages where the thick convective envelope has been developed, analogous to the asymptotic giant branch (AGB) stage of Population I/II stars. Middle panel: the He core mass for stars with thick convective envelopes (cyan lines in the upper panel). The dredge-up processes may happen in the convective regions and reduce the He core mass. The minimum and maximum He core masses at the AGB stages are shown in black circles and red triangles, respectively. The black solid line represents the logarithm interpolation between the maximum and minimum values of He core masses, which gives the typical WD progenitor mass for a given WD. Lower panel: the typical evolutionary timescale of the progenitor stars. The timescales are calculated from ZAMS stages to the bottom of the AGB stage (the lower ends of the cyan lines).