adsabs/AstroCLIMB huggingface dataset:
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Petersen diagram of multimode δ Sct stars. The period ratio (y-axis) is the short period (P  S ) divided by the long period (P  L ) .
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Petersen diagram of 1O/F double-mode δ Sct stars. The period ratio (y-axis) is the 1O-mode period divided by the F-mode period.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Color–magnitude diagram of our sample. Single stars, binaries, and YSOs are shown with gray, red, and blue points, respectively.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: (a) Mass-loss rate of the planetary primordial atmospheres induced by X-ray emission. The mass-loss rate within 0.1 and 1 Gyr is plotted with black and purple horizontal lines, respectively. Stars above the lines suggest they can remove the planetary primordial envelopes within 0.1 or 1 Gyr. Different colors represent different effective temperatures. The Sun is denoted by a black star. (b) Mass-loss rate of planetary atmospheres induced by stellar X-ray emission, which has been corrected to a younger age.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Left panel: Activity–rotation relation of binaries. The gray and coral dots are from Wright et al. (2011) and this work, respectively. The Ro from Wright et al. (2011) are shifted by a factor of Ro/3. The magenta line is our best-fit result. Right panel: Comparisons of activity–rotation relations from different studies. The shaded region shows 100 models extracted randomly from the posterior probability distribution.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: (a) Toomre diagram of dwarfs and ultraluminous sources. (b) Toomre diagram of binaries and YSOs. (c) Galactic distribution of dwarfs and ultraluminous sources. z is the vertical distance to the Galactic plane. R gc is the radial distance to the Galactic center. (d) Galactic distribution of binaries and YSOs.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Activity–rotation relations of F-, G-, K-, and M-type binary stars, respectively. Binaries are categorized using the same criteria given in the caption of Figure 4. The magenta dashed lines are the best-fit activity–rotation relation shown in Figure 6.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Comparison of R  X  of common targets between this work and Wright et al. (2011). Different colors represent different effective temperatures.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Fine structures of the activity–rotation relation of single stars. “S” represents the supersaturation region. The first “D” represents the weak decay region while the second one corresponds to the fast-decay region. “F” stands for the region with an almost flat slope.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Comparison of R  X  of common targets between various works and Freund et al. (2024). Different colors represent sources from different literature.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: (a) Posterior distributions of parameters of the piece-wise power law for single stars. (b) Posterior distributions of parameters of the piece-wise power law for binaries.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The continuum-calibration process. (a) The black line represents the normalized spectrum, and the orange line corresponds the template spectrum, which is the nearest in the parameter space. The stellar parameters of this template spectra are T eff  =  5800 K, ﹩\mathrm{log}g=3.00\,\mathrm{dex}﹩, and [Fe/H]  =   −0.60 dex. (b) The green crosses denote the quotient data points obtained by dividing the observed spectrum by the template one. The purple line is the curve fitted using local polynomial regression. (c) By dividing the normalized spectrum by the fitting curve, we calibrate the normalized continuum of the LAMOST-MRS spectrum.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The normalized synthetic spectra with different S/N. The stellar parameters of these synthetic spectra are T eff  =  5800 K, ﹩\mathrm{log}g=4.50\,\mathrm{dex}﹩, and [Fe/H]  =  0.0 dex, and the wavelength range and resolution are the same as LAMOST-MRS. (a) The gray and black lines are the spectra with S/N = 20 and 100, respectively. The green and purple lines indicate the pseudocontinuums of these spectra, which are normalized by the continuum-fitting method. (b) The green and purple lines are the same as in panel (a), representing the pseudocontinuums. The black lines are the synthetic spectra without noise.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The blue and red arm spectra of a double-line spectroscopic binary system. The spectral lines are split due to the RV difference between the companion stars of the binary system.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: Flowchart.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distributions of Gaia G magnitude vs. S/N of the LAMOST-MRS blue (upper panel) and red arm (lower panel) spectra.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Upper left: flowchart schematic illustrating the  NuSTAR   data-processing steps undertaken to reduce individual fields for the serendipitous survey. A field can comprise multiple exposures (obsIDs) mosaicked into a single counts image, as illustrated on the right. Data from the two telescopes, FPMA  and FPMB, and the coadded FPMA+B are indicated as “A”, “B,” and “C”, respectively, and the three energy bands are indicated in different colors (3−8 keV, 8−24 keV, and 3−24 keV). Upper right: example of real counts images and exposure maps associated with stages (iii)–(v) for one of the included processed fields, i.e., IC 2560. The data shown are for the coadded images and the 3−24 keV energy band only. This illustrates the mosaicking of two exposures with different exposure times and orientations. Information from both the image and the exposure map mosaics is used to perform source detection (step (iv)). In this example, three serendipitous sources (circled) are detected. Lower: each image mosaic with counts <1 × 106 is visually assessed to identify regions with excess background contamination (EBC), which includes stray light, ghost rays, aperture background, and bright science target. If less than two-thirds of the image is contaminated by excess background, a mask region is created and used to mask detections from the final source list. Images with counts >1 × 106 or with EBC covering more than two-thirds of the image are excluded from the catalog (38 exposures were removed in this way).
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: The average exposure time (blue circles) and the number of  NuSTAR   exposures (green stars) roughly per semester over the full 80 month period. In general, the average exposure time shows little variation between the 40 month (shaded gray area) and post-40 month observations, while we see an increase in the number of exposures from the 40 month to the post-40 month survey, resulting in an increase in the total exposure time per semester which can be utilized for the  NuSTAR   serendipitous survey. In total, the 80 month serendipitous survey includes 1457 individual exposures with a cumulative exposure time of 62 Ms.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Sky coverage (solid angle) of the NSS40 (blue) and NSS80 (green) surveys as a function of aperture-corrected flux sensitivity, for the three main energy bands, i.e., full (3−24 keV), soft (3−8 keV), and hard (8−24 keV). Note the factor of ∼3 increase in the sky coverage with  NuSTAR   between the 40 month and 80 month catalogs. The sensitivity curves include fields at all Galactic latitudes for both NSS40 and NSS80 (see the curves shown in L17 for both the full survey and the subset of fields that lie outside the Galactic plane, ∣b∣ > 10°).
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Aitoff projection showing the distribution of the  NuSTAR   serendipitous survey fields on the sky, in Galactic coordinates. The white and color-filled circles show the NSS40 and the post-NSS40 data, respectively. The circle sizes correspond to the number of sources detected in a given field, and the colors correspond to the cumulative exposure time (per FPM) for a given field. The white area highlights the region ±10° of the Galactic plane.
Paper: Observations of Five Major Uranian Satellites during 2013–2020 Based on Gaia DR3
Authors: H. Y. Zhang, Y. Yu, R. C. Qiao, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: The residual distribution of the five major Uranian satellites under the exposure times of 30, 60, and 120 s are shown. Each row represents the O − C residual distribution in the R.A. and decl. directions of a specific satellite, observed on 2013 October 10.
Paper: Observations of Five Major Uranian Satellites during 2013–2020 Based on Gaia DR3
Authors: H. Y. Zhang, Y. Yu, R. C. Qiao, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: Example of this observation experiment viewed on 2013 October 10. Panel (a) is the original image and panel (b) is the preprocessed image. U1, U2, U3, U4, and U5 represent the five major Uranian satellites (Ariel, Umbriel, Titania, Oberon, and Miranda, respectively).
Paper: Observations of Five Major Uranian Satellites during 2013–2020 Based on Gaia DR3
Authors: H. Y. Zhang, Y. Yu, R. C. Qiao, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: Offsets (O − C) vs. time of the major Uranian satellites in R.A. and decl. for the six observation missions from 2013 to 2020. Offsets are computed from the comparison of our observations to the ephemerides of DE441 for Uranus and Lainey et al. (2015) for satellites.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The visualization of 2D slices of downgraded fields constructed by the CIC (top), CIC+GS (middle), and DTFE (bottom) methods. As a reference, the noise-free field constructed by the CIC method is also presented in the top left panel. Except for this panel, the left, middle, and right panels represent the 1%, 0.1%, and 0.01% downgraded fields, respectively. All these fields are created by using N g = 10243 grid cells within a box of size L = 600 h −1 Mpc. Each 2D slice displays the same region of the simulation box, with the same projection depth of 5.27 h −1 Mpc. For the CIC+GS case, the smoothing lengths of R G = 2.93 h −1 Mpc, R G = 5.86 h −1 Mpc, and R G = 11.72 h −1 Mpc are adopted for the 1%, 0.1%, and 0.01% downgraded fields, respectively (see Appendix A). In comparison with the top left panel, the top panels display the emergence of discreteness in the CIC DM fields, as the particle number density is successively downgraded. These severe discreteness effects will hamper proper morphological measurements of LSS with MFs (see Figure 1). The middle panels display the continuous downgraded fields obtained by using CIC+GS method. This method inevitably destroys large amounts of the intrinsic structural elements of LSS by introducing excessive smoothing. Therefore, it will significantly diminish the morphological information contents captured by MFs. The bottom panels show the continuous downgraded fields constructed by using the DTFE method. Benefiting from the anisotropic and spatial self-adaptive feature, DTFE can help introduce minimum smoothing and retain the intrinsic structural elements of LSS to the maximum extent possible. Compared with the CIC+GS method, DTFE can greatly improve the morphological information contents captured by MFs (see Figure 3).
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The MFs of the noise-free field and two 1% downgraded fields, where the noise-free field is constructed by the CIC method and the two 1% downgraded fields are constructed by the CIC+GS and DTFE methods, respectively (see Figure 2). For the CIC+GS case, the smoothing length adopted is R G = 2.93 h −1 Mpc. As we can see, the amplitudes of the DTFE MFs of the 1% downgraded field (i.e., the red lines) are very close to those of the CIC MFs of the noise-free field (i.e., the bold green lines; also see Figure 1). This means that DTFE indeed can help retain intrinsic structural elements of LSS. The amplitudes of the CIC+GS MFs (i.e., the blue lines) are much lower than those of the MFs in other two cases. This is because the CIC+GS scheme erases large amounts of intrinsic structural elements of LSS. Note that these results are plotted with a logarithmic y-axis to better visualize the MFs in the CIC+GS case.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The MFs of the noise-free field and the 10%, 1%, and 0.1% downgraded fields, which are constructed by the CIC method with N g = 10243 grid cells. They are represented by bold green lines and red, blue, and yellow lines, respectively. Here, the bold green lines can be treated as the ideal LSS MFs, without discreteness effects. By comparing the lines with different colors, this plot demonstrates how discreteness affects the measurements of MFs.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The DTFE MFs of uniform-weighted halo fields with various grid resolutions in real space. The corresponding halo number density for these fields is ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩. The blue, red, and green lines correspond to halo fields with N g = 10243, N g = 20483, and N g = 40963 grid cells, respectively. As shown, the amplitudes of V 1, V 2, and V 3 become greater as N g increases. This means that under the DTFE scheme, a higher grid resolution can help resolve more subtle structural elements from the point set.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The DTFE MFs of uniform-weighted halo fields with various halo number densities in real space. The green, red, and blue lines correspond to halo number densities of ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, ﹩1.6\times {10}^{-3}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, and ﹩1.6\times {10}^{-4}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, respectively. The amplitudes of the MFs decrease with the decrease of the halo number density, indicating information losses in lower-halo-number-density cases.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The visualization of 2D slices of differently weighted DTFE halo fields in real space. The corresponding halo number density for these fields is ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩. From left to right, each panel corresponds to the uniform-weighted, mass-weighted, and optimally weighted halo fields, respectively. Each slice shows the same ﹩1200\times 1200{({h}^{-1}\,\mathrm{Mpc})}^{2}﹩ region, with 10.55 h −1 Mpc thickness of the simulation box.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The MFs of the noise-free field and various downgraded fields under different smoothing lengths. Left panels: the MFs of the noise-free field (blue lines) and 1% (green lines), 0.1% (yellow lines), and 0.01% (red lines) downgraded fields, under R  G  = 5L  g  = 2.93 h −1 Mpc. Middle panels: the MFs of the noise-free field (blue lines) and 0.1% (green lines), 0.01% (yellow lines), and 0.001% (red lines) downgraded fields, under R  G  = 10L  g  = 5.86 h −1 Mpc. Right panels: the MFs of the noise-free field (blue lines) and 0.01% (green lines), 0.001% (yellow lines), and 0.0001% (red lines) downgraded fields, under R  G  = 20L  g  = 11.72 h −1 Mpc. Here, ﹩{L}_{g}=L/{N}_{g}^{1/3}\simeq 0.59\,{h}^{-1}\,\mathrm{Mpc}﹩ is the grid cell size. The shaded bands show 1σ scatters. As shown, the MFs of the 1%, 0.1%, and 0.01% downgraded fields under smoothing lengths of R  G  = 2.93 h −1 Mpc, R  G  = 5.86 h −1 Mpc, and R  G  = 11.72 h −1 Mpc overlap with the MFs of the noise-free field under the corresponding smoothing lengths, respectively, within the 1σ accuracy range. That is, in each panel, the green line basically overlaps with the blue line. This means that under these smoothing lengths, the shot noise effects on the MFs of the corresponding downgraded fields can be sufficiently smoothed out. As the downgrading level increases, these smoothing lengths are inadequate to eliminate shot noise effects on the MFs. Consequently, in each panel, the yellow and red lines deviate from the blue line, illustrating how shot noises affect the measurements of CIC+GS MFs.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The RSD signals and corresponding S/Ns of the MFs. The RSD signals are obtained by measuring the differences between the MFs of uniform-weighted halo fields in redshift space and real space (i.e., ΔV i ; see Equation (18)). The S/Ns are calculated through ﹩\left|{\rm{\Delta }}{{\rm{V}}}_{i}\right|/{\sigma }_{i}﹩, where σ  i  is the 1σ error on ΔV  i . From the left to right columns, the results for V 0, V 1, V 2, and V 3 are presented, respectively. From top to bottom, each row corresponds to cases of the halo number density of ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, ﹩1.6\times {10}^{-3}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, and ﹩1.6\times {10}^{-4}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, respectively. For each panel, the top subplot shows the RSD signals and the bottom subplot presents the RSD S/Ns, where the blue and red curves are for the CIC+GS and DTFE cases, respectively. In the CIC+GS case, for halo number densities in descending order, the smoothing lengths R  G  = 6.8 h −1 Mpc, R  G  = 14.6 h −1 Mpc, and R  G  = 31.4 h −1 Mpc are adopted, respectively. These smoothing lengths are determined by the mean halo spacings of our halo samples. The shaded band shows the 1σ scatter.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The Fisher error forecasts for the structure growth rate, with n b = 32 (see Appendix C for technical details). The results for the CIC+GS and DTFE MFs are marked with blue circles and red diamonds, respectively. As shown, the y-axis values of the red diamonds are much lower than those of the blue circles by a factor of around 3–5. This means that compared with traditional CIC+GS MFs, the DTFE MFs are more sensitive to cosmological parameters, because they contain more morphological information of LSS.