adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Core groups used in this study. Total ALMA-IMF cores detected in getsf are first divided into two groups by the criteria passing a robust 1.3 mm detection or a robust 1.3 mm and 3 mm detection in the getsf core catalog. The core samples are further classified into two groups by examining the spatial overlap with the high-res continuum images. The number of cores in each group is listed in parentheses. Each group used in the analyses of this study is labeled.
Paper: Morphological Regimes of Rotating Moist Convection
Authors: Whitney T. Powers, Adrian E. Fraser, Evan H. Anders, Jeffrey S. Oishi, Benjamin P. Brown
Figure caption: Panel (a): volume-averaged Reynolds number plotted against Rossby number for simulations at constant values of Rayleigh number (circles and upward/downward triangles) as well as simulations with constant RaEk4/3 (squares and a dashed line). Panel (b): volume-averaged moist Nusselt number plotted against Rossby number for the same sets of simulations. The dynamical regimes are identified by color, with cells in green, funnels in orange, and plumes in blue. The dotted lines show the values for nonrotating simulations at each of the three constant Rayleigh number cuts.
Paper: Multiphase Gas Offsets in the Atmospheres of Central Galaxies and Their Consequences for SMBH Activation. I. The Hot and Warm Ionized Gas Phases
Authors: Francesco Ubertosi, Fabrizio Brighenti, Ewan O'Sullivan, Gerrit Schellenberger, Myriam Gitti, Simona Giacintucci, Pasquale Temi, Laurence P. David, Jan Vrtilek, Tiziana Venturi, Elisabetta Liuzzo, Marcella Massardi, Kamlesh Rajpurohit
Figure caption: Multiwavelength views of the systems in our sample. The panels show smoothed X-ray Chandra maps of the hot gas, with grayscale contours of the Hα line from MUSE data. The red square marks the position of the X-ray peak, the purple circle shows the location of the Hα peak, and the black star shows the position of the SMBH (see Table 1). When detected, the VLBA image of the parsec-scale radio core is shown in the insets.
Paper: Multiphase Gas Offsets in the Atmospheres of Central Galaxies and Their Consequences for SMBH Activation. I. The Hot and Warm Ionized Gas Phases
Authors: Francesco Ubertosi, Fabrizio Brighenti, Ewan O'Sullivan, Gerrit Schellenberger, Myriam Gitti, Simona Giacintucci, Pasquale Temi, Laurence P. David, Jan Vrtilek, Tiziana Venturi, Elisabetta Liuzzo, Marcella Massardi, Kamlesh Rajpurohit
Figure caption: BPT diagram of the systems in our sample from MUSE data, showing the line ratio ﹩{\mathrm{log}}([{\rm{O}}\,{\rm{III}}]\,\lambda 5007/{\rm{H}}\beta )﹩ vs. ﹩{\mathrm{log}}([{\rm{N}}\,{\rm{II}}]\,\lambda 6583/{\rm{H}}\alpha )﹩ for spaxels with SNR > 3 in all four lines. Systems that do not fulfill this requirement in any spaxel are marked. The standard demarcation curves from L. J. Kewley et al. (2001; K01), G. Kauffmann et al. (2003; K03), and R. Cid Fernandes et al. (2010; CF10) are overlaid to distinguish between regions dominated by star formation, AGN photoionization, composite activity, and LINER-like excitation. The position of the Hα peak is highlighted with a red star. The sizes of the black points are proportional to their Hα intensity. The subplot to the left shows the Hα intensity (black contours) and the subset of spaxels with SNR > 3 in all four lines (colors). The absence of points in the AGN region confirms that the warm-gas emission is not dominated by AGN photoionization, supporting the interpretation of a non-AGN origin for the ionization near the Hα peak. From left to right, top to bottom: NGC 5846, NGC 5044, A3581, NGC 7237, A496, A2052, ZwCl 0335+096, A1644, A2626, A85, A133, A1991, A2495, A478, MCXC J1558.3-1410, PKS 0745-191, RXJ 0821.0+0752, A1664, RXJ 1350.3+0940, MCXC J2014.8-2430, A383, and MCXC J0331.1-2100.
Paper: What Can We Learn about Reionization Astrophysical Parameters Using Gaussian Process Regression?
Authors: Purba Mukherjee, Antara Dey, Supratik Pal
Figure caption: Evolution of the ionization fraction (QH II) and global 21 cm signal (ΔTb) from reconstruction. Plots (a) and (b) show the ionization fraction obtained using UV17+QHII+Planck (blue curve) versus UV17+QHII+Planck for a fixed value of the clumping factor CH II = 5 (red dashed line) from the GP reconstruction of the UV luminosity density with the UV17(A) (left panels) and UV17(B) (right panels) compilations. Plots (c) and (d) show the global 21 cm signal at the reionization epoch from respective data sets. The QHII data are plotted with references for comparison. Mock A and B represent the simulated ΔTb versus z catalogs.
Paper: What Can We Learn about Reionization Astrophysical Parameters Using Gaussian Process Regression?
Authors: Purba Mukherjee, Antara Dey, Supratik Pal
Figure caption: Comparison between the constraints obtained on the astrophysical parameters employing (a) UV17(A)+QHII versus UV17(B)+QHII, (b) with the clumping factor kept constant at CH II = 5, (c) UV17(A)+QHII+Planck versus UV17(B)+QHII+Planck, and (d) with the clumping factor kept constant at CH II = 5 during the MCMC. The black dashed line and shaded region represent the Planck best fit with 1σ CL.
Paper: What Can We Learn about Reionization Astrophysical Parameters Using Gaussian Process Regression?
Authors: Purba Mukherjee, Antara Dey, Supratik Pal
Figure caption: Comparison between the bounds obtained on the astrophysical parameters using UV17(A)+QHII+Planck+SARAS versus UV17(B)+QHII+Planck+SARAS and (b) with a constant clumping factor of CH II = 5 (panel (b)). Evolution of the ionization fraction in (c) and the global 21 cm signal at the reionization epoch in (d) were obtained using UV17(A)+QHII+Planck+SARAS (blue curve) and UV17(B)+QHII+Planck+SARAS (red dashed line) from the GP reconstruction of the UV luminosity density with the UV17(A) and UV17(B) compilations, respectively.
Paper: What Can We Learn about Reionization Astrophysical Parameters Using Gaussian Process Regression?
Authors: Purba Mukherjee, Antara Dey, Supratik Pal
Figure caption: The reconstructed UV luminosity density function in the redshift range z ∼ 4–12 obtained from GPR using the UV17(A) and UV17(B) data.
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: Time profiles of flux density at the eight RSTN frequencies (top panel) and Wind/Waves at 1 MHz (bottom) for three ≥M5 SXR flare counterexamples from 2011–2016 to the dominant classification dichotomy found in this study, for which flares with low-frequency cutoffs in their peak-flux-density microwave spectrum were confined, and flares with emission that extended to 410 MHz were eruptive. Event (a) was plausibly associated with a jet-type CME (see text) while events (b) and (c) may be cases in which an initially confined flare triggered a CME. The dashed vertical lines indicate the time of peak 4995–15,400 emission (top panel) and the onset and peak of 1–8 Å SXR emission (bottom).
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: (Top panel for each event) Time profiles of flux density at the eight RSTN frequencies for eight ≥M5 CME-associated flares from 2011 to 2016. (Middle) Associated 1 MHz intensity-time profiles. (Bottom) 1–15,400 MHz peak-flux-density spectra. In all cases, the low-frequency emission at the time of peak high-frequency emission flux extends downward to 410 MHz. The dashed lines indicate the time of peak 4995–15,400 emission (top panel) and the onset and peak of 1–8 Å SXR emission (middle).
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: Scatter plot of the peak flux in the 4995–15,400 MHz range vs. the peak 410 MHz flux for samples of confined (Table 2; red data points) and eruptive ≥M5 SXR flares (from Tables 1 and 3; blue). To first order, the dashed vertical line at 10 sfu separates the two populations. The labels refer to table and list numbers for four counter examples to the microwave spectral classification dichotomy of confined and eruptive solar flares.
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: Histogram of the peak Wind/Waves 1 MHz emission for the confined and eruptive ≥M5 flares in this study that were observed by Wind/Waves.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Nd II abundance calculations based on observed lines for the Sun (top) and HD 222925 (bottom) for LTE and NLTE models with different SH factors, compared to published A(Nd) values (shown as blue shaded regions). Vertical axis labels indicate whether the HM model or a MARCS model atmosphere were used for the different SH factors. Orange lines show the median of the line-by-line Nd abundances, while green triangles show the mean. The lower and upper boundaries of the boxes represent the first and third quartiles of the line-by-line abundances, respectively, with outliers shown as black circles.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Grotrian diagrams of Nd II for three model atoms: atom A (top), atom B (middle), and atom C (bottom; see Section 2.4 for details on the atoms). Dotted lines indicate the ground state and ionization energy of Nd II. The 122 transitions of interest shown in Figure 1 are also highlighted here in red. Transitions are highlighted in blue if their lower energy level is theoretical.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Grotrian diagrams of Nd I and Nd II displaying all energy levels and bound–bound transitions as generated by FORMATO3. Spectral line data were assembled from VALD, NIST, Linemake, and S. Hasselquist et al. (2016). Dotted lines indicate the ground state and ionization energy of each species, and 122 transitions of interest that have been previously observed in stellar spectra are highlighted in red.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: COGs for two Nd II lines generated with MULTI2.3 using the solar MARCS model. Measured EWs from E. A. Den Hartog et al. (2003) were converted into A(Nd) values in both NLTE (dark blue) and LTE (light orange) by interpolating from a cubic best-fit curve.
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: (Top panel for each event) Time profiles of flux density at the eight RSTN frequencies for the eight confined X-class flares from NOAA AR 12192. In each case, the low-frequency emission at the time of peak high-frequency microwave flux is cut off at a frequency ≥410 MHz. (Middle) Time trace of Wind/Waves 1 MHz emission. (Bottom) 1–15,400 MHz peak flux radio spectra for each event, with the 1 MHz peak flux plotted in red on the y axis (see text for explanation of the two 1 MHz values in (a), (e), and (h)). The dashed lines indicate the time of peak 4995–15,400 MHz emission (top panel) and the onset and peak of 1–8 Å SXR emission (middle).
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: (Top panel for each event) Time profiles of flux density at the eight RSTN frequencies for the four eruptive flares from NOAA AR 12192. (Middle) Wind/Waves 1 MHz time traces. (Bottom) Composite radio spectrum for each event from 1 to 15,400 MHz. The dashed lines indicate the time of peak 4995–15,400 MHz emission (top panel) and the onset and peak of 1–8 Å SXR emission (middle).
Paper: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Authors: E. W. Cliver, M. Kazachenko, H. S. Hudson, T. Alberti, M. Laurenza, S. M. White, P. T. Gallagher
Figure caption: An unusual microwave burst (No. 5 in Table 2) with a cutoff spectrum and a significant (∼9000 sfu) 1 MHz burst.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: NLTE corrections as a function of A(Nd)LTE (top left) and [Fe/H] (top right). Five commonly measured optical lines (4061.080, 4109.447, 4462.979, 5255.504, and 5319.813 Å) and three H-band lines (15368.118, 16053.616, and 16262.042 Å) are shown in each graph. With the exception of the parameter being varied, the dark red lines were calculated with typical red giant parameters (Teff = 4250 K, ﹩{\mathrm{log}}\,g﹩ = 1.50, [Fe/H] = −2.0, ξt = 2.0 km s−1, and A(Nd) = −0.50) and light blue lines were calculated with typical dwarf parameters (Teff = 5750 K, ﹩{\mathrm{log}}\,g﹩ = 4.30, [Fe/H] = −2.0, ξt = 1.0 km s−1, and A(Nd)LTE = −0.50). The bottom panels show the same data points as the top panels, but with REW plotted on the horizontal axis. A lower limit of ﹩\mathrm{log}({\rm{EW}}/\lambda )=-7.5﹩ is chosen to make the effects of saturation above ﹩\mathrm{log}({\rm{EW}}/\lambda )\gtrsim -5.0﹩ more visible.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Departure coefficients as a function of optical depth at 5000 Å. The left and middle columns of panels show departure coefficients for the lower (solid) and upper (dashed) levels of a near-UV, optical, and NIR spectral line, for model atmospheres of a typical dwarf (Teff = 5750 K, ﹩{\mathrm{log}}\,g﹩ = 4.3, and ξt = 1 km s−1) and giant (Teff = 4250 K, ﹩{\mathrm{log}}\,g﹩ = 1.5, and ξt = 2 km s−1). The top right and bottom right panels show departure coefficients for a single optical line (5319 Å, EP = 0.55 eV) in both models at five different values of A(Nd).
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Heat maps of ΔANLTE for six Nd II lines across the optical and NIR. Each individual panel in each heat map shows variations with Teff and ﹩{\mathrm{log}}\,g﹩ for a specific combination of [Fe/H] and A(Nd)LTE as indicated by the labels surrounding the panel. A value of ξt = 1.5 km s−1 is interpolated for all heat maps. Corrections are omitted if the interpolated model atmosphere was unreliable, or if the REW does not fall in the range ﹩-7.0\leqslant \mathrm{log}({W}_{\lambda }/\lambda )\leqslant -4.5﹩.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Plots of ΔANLTE as a function of both wavelength (top) and EP (bottom) for 16 different combinations of stellar parameters [Fe/H], Teff (K), ﹩{\mathrm{log}}\,g﹩, and A(Nd)LTE near different extremes of the grid (indicated within each plot). We adopt ξt = 2 km s−1 for giant stars (﹩{\mathrm{log}}\,g﹩ = 1.5) and ξt = 1 km s−1 for dwarf stars (﹩{\mathrm{log}}\,g﹩ = 4.5). Hotter giant stars with the clearest negative trends are in the lower left quadrant. As with Figure 11, corrections are omitted if ﹩\mathrm{log}({W}_{\lambda }/\lambda )\lt -7﹩ or ﹩\mathrm{log}({W}_{\lambda }/\lambda )\gt -4.5﹩.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Observed and synthetic spectra for wavelength regions around two solar Nd II lines (top) and two Nd II lines in HD 222925 (bottom). For HD 222925, the abundances were obtained and synthetic spectra were generated using the stellar parameters listed in I. U. Roederer et al. (2018). Shaded regions indicate ±0.2 dex in the NLTE abundance. Prominent spectral lines and features are labeled. Small panels above each plot are zoomed in on the Nd II lines under consideration.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Comparison of ΔANLTE calculation methods for 248 measurements of optical Nd II lines in FGK stars. Interpolated points are shown as green circles, and extrapolated points are shown as purple triangles. A shaded region is included to highlight points that are within 0.01 dex of exact agreement. Residuals from the one-to-one line are shown (μ = 0.00140, σ = 0.00393) with shaded regions indicating ±1σ and ±2σ.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: A grid displaying all values of A(Nd)LTE chosen for each metallicity value in our parameter space (−3.0 ≤ [Fe/H] ≤ −1.0). A line showing [Nd/Fe] = 0 is provided for reference.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Line-by-line A(Nd) vs. EP (top) and REWs (bottom) for HD 115444, with lines of best fit for both LTE and NLTE (slopes given in the legend). The LTE abundance is A(Nd)LTE = −1.155 ± 0.079, and the NLTE abundance is A(Nd)NLTE = −0.910 ± 0.073.
Paper: Investigating Non-LTE Abundances of Neodymium in Metal-poor FGK Stars
Authors: John D. Dixon, Rana Ezzeddine, Yangyang Li, Thibault Merle, Manuel Bautista, Yanjun Guo
Figure caption: Plots of ΔANLTE vs. [Fe/H] (top), ﹩{\mathrm{log}}\,g﹩ (middle), and Teff (bottom) for the stars in Table 3. Each point represents the mean ΔANLTE value calculated using spectral line measurements from a single paper.
Paper: Resolved Profiles of Stellar Mass, Star Formation Rate, and Predicted CO-to-H2 Conversion Factor Across Thousands of Local Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, I-Da Chiang, 宜達 江, Adam K. Leroy, Karin Sandstrom, Jakob den Brok, Alberto D. Bolatto, Jérémy Chastenet, Ryan Chown, Annie Hughes, Eric W. Koch, Thomas G. Williams
Figure caption: Galaxy distribution and the predicted global αCO values across the M⋆–SFR plane. Top left: Two-dimensional histogram (grayscale heatmap) and iso-density contours (dashed curves) of galaxies in our sample. Their distribution mostly centers around the SFMS at z ≈ 0 (blue line; A. K. Leroy et al. 2019). Top middle and right: Predicted galaxy global αCO(1−0) and αCO(2−1) values across the same plane (overlaid with the same density contours as in the top left panel). The highest αCO values appear at the low M⋆ end, and the lowest αCO values appear at higher M⋆ and away from the SFMS. Bottom: Variations of the CO-dark, emissivity, and line ratio terms in the SL24 αCO prescriptions. These variations work in concert to drive the systematic trends seen in αCO in the top middle and right panels. Note that the colorbar for R21 (bottom right) is reversed so that brighter colors still imply lower αCO as in other panels.
Paper: Resolved Profiles of Stellar Mass, Star Formation Rate, and Predicted CO-to-H2 Conversion Factor Across Thousands of Local Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, I-Da Chiang, 宜達 江, Adam K. Leroy, Karin Sandstrom, Jakob den Brok, Alberto D. Bolatto, Jérémy Chastenet, Ryan Chown, Annie Hughes, Eric W. Koch, Thomas G. Williams
Figure caption: Galaxy-integrated SFR to CO luminosity ratios as a function of stellar mass (top) and the implied molecular gas depletion time trends (bottom). Results based on CO (1–0) data are shown on the left, whereas those based on CO (2–1) are on the right. In the top panels, blue/orange symbols show a large set of observational measurements (diamonds) and CO upper limits (upward triangles, corresponding to ﹩\mathrm{SFR}/L{{\prime} }_{\mathrm{CO}}﹩ lower limits) from the literature compiled by A. K. Leroy et al. (2022, 2023). The blue/orange solid lines show the running median for these observations, and shaded regions showing the 1σ (16–84th percentile) range. Gray symbols and dotted lines instead show the expected relationship across our sample from our predicted global αCO values assuming a fixed molecular gas depletion time tdep, fid = 2 Gyr. The discrepancies between the observations (blue/orange) and the expectations (gray) can be explained if tdep varies systematically as a function of M⋆. We show these implied variations in the bottom panels. The implied tdep variations are ∼0.5 dex across the probed M⋆ range and 0.1–0.3 dex at a given M⋆.
Paper: Resolved Profiles of Stellar Mass, Star Formation Rate, and Predicted CO-to-H2 Conversion Factor Across Thousands of Local Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, I-Da Chiang, 宜達 江, Adam K. Leroy, Karin Sandstrom, Jakob den Brok, Alberto D. Bolatto, Jérémy Chastenet, Ryan Chown, Annie Hughes, Eric W. Koch, Thomas G. Williams
Figure caption: Effects of finite data resolution on galaxy half-light radius (r50) measurements. The y-axes show the discrepancy between the observed half-light radius (r50, obs) and the true value (r50, true), which diminishes as the galaxy becomes better resolved (toward larger x values). The x-axis represents the ratio of galaxy exponential scale radius (rscale, true) over PSF size (θPSF) in the left panel, or the ratio of the observed effective radius (r50, obs) over PSF size in the right panel. When measuring r50 with the direct radial binning method (see Section 2.2), resolution-induced discrepancies are more substantial for more inclined galaxies (brighter colored lines); in contrast, r50 measured via the stripe integral method (see Section 2.2 and Appendix A) is insensitive to galaxy inclination. Results shown in the right panel can be used to correct for resolution-induced biases in r50 because both r50, obs/θPSF (x-axis) and i (color-code) are directly measurable from observations.
Paper: Resolved Profiles of Stellar Mass, Star Formation Rate, and Predicted CO-to-H2 Conversion Factor Across Thousands of Local Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, I-Da Chiang, 宜達 江, Adam K. Leroy, Karin Sandstrom, Jakob den Brok, Alberto D. Bolatto, Jérémy Chastenet, Ryan Chown, Annie Hughes, Eric W. Koch, Thomas G. Williams
Figure caption: Illustration of a surface brightness profile measured from radial binning (I1, I2, . . . , In; top) and a flux density sequence computed via stripe integrals (S1, S2, . . . , Sn; bottom). For axisymmetric disks, they are related by a discrete version of the Abel transform (or its inverse).