adsabs/AstroCLIMB huggingface dataset:
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: The decision process used to determine if a pixel is black, white, or colored in the fractional polarization maps. A colored pixel indicates a detection with color indicating the fractional polarization. A black pixel indicates an upper limit to the fractional polarization ≤1%. A white pixel represents no information.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: THOR+VGPS map of SNR G43.3−0.2 at 1420 MHz. Contour levels are Stokes I (black) at 60, 160, 260, 400, 700, and 900 mJy beam−1. The red box indicates the region in which a grid search was done for polarization and Faraday rotation. Included in this image is the H II region W49N at G043.1658+00.0118 (Dreher et al. 1984; Anderson et al. 2018). W49A is included in this figure for reference because it is used in the analysis of polarization leakage outlined in the Appendix.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Faraday depth map of SNR G39.2 − 0.3. Contours are from the THOR+VGPS map at 20, 30, 55, 80, 110, and 140 mJy beam−1. The red boxes are identified as Region 1 and Region 2 where the Faraday depth spectra are shown as grid plots in Figures 19 and 20. The subregions with a purple edge indicate the locations of two-component of Faraday rotation. The Faraday rotation shown for subregions with two-component Faraday rotation is derived from the strongest peak.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Grid plot of the Faraday depth spectra for Region 2 seen in Figure 18. The horizontal limits and gray region are the same as described in Figure 6. The red horizontal line is our detection threshold P = 0.30 mJy. See Figure 6 for a description of the blue, purple, and black profiles. The coordinates of the bottom-left and top-right corners are (ℓ, b) = (39.°265, −0.°374), and (ℓ, b) = (39.°235, −0.°344). Using the distance of 9.5 ± 0.1 kpc derived in Lee et al. (2020), the physical size of the region we show as a grid plot is 4.97 ± 0.05 pc on each side.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Grid plot of the Faraday depth spectra for Region 1 seen in Figure 18. The horizontal limits and gray region are the same as described in Figure 6. The red horizontal line is our detection threshold P = 0.30 mJy. See Figure 6 for description of the blue and black profiles. The coordinates of the bottom-left and top-right corners are (ℓ, b) = (39.°257, −0.°329) and (ℓ, b) = (39.°227, −0.°299). Using the distance of 9.5 ± 0.1 kpc derived in Lee et al. (2020), the physical size of the region we show as a grid plot is 4.97 ± 0.05 pc on each side.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: THOR+VGPS map of SNR G39.2 − 0.3 at 1420 MHz. Contour levels (green) at 20, 30, 55, 80, 110, and 140 mJy beam−1. The red box indicates the region in which a grid search was done for polarization and Faraday rotation. The extended source outside of the red box is identified from THOR as the H II region G039.280 − 00.003 (Anderson et al. 2018; Wang et al. 2018).
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Distribution of Faraday depth for all peaks above our detection threshold. The purple, orange, green and blue bars represent the first-, second-, third-, and fourth-highest peaks. The black curve is the RMSF shifted to the average Faraday depth of the cluster with the highest peak and scaled to the peak value.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Faraday depth map of the SNR G43.3−0.2 for the positive components (a) and negative components (b). Contour levels are 60, 160, 260, 400, 700, and 900 mJy beam−1. The subregions with a purple edge indicate the locations with two-component Faraday rotation. The Faraday rotation shown for subregions with two-component Faraday rotation is derived from the strongest peak.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: THOR+VGPS map of SNR G41.1 − 0.3 at 1420 MHz. Contour levels are for Stokes I (green) at 25, 50, 150, 200, 300, and 350 mJy beam−1. The red box indicates the region that a grid search was done for polarization and Faraday rotation. The source outside of the red box is identified from THOR as the H II region G041.101-00.221 (Anderson et al. 2018; Wang et al. 2018).
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Fractional polarization map of the SNR G43.3 − 0.2 with contour levels (green) at 60, 160, 260, 400, 700, and 900 mJy beam−1 from THOR+VGPS. The process by which colored and black subregions are defined is shown in Figure 8. The pixel color corresponds to the fractional polarization found from the highest peak in the Faraday depth spectrum for each subregion.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Fractional polarization map of SNR G41.1 − 0.3. The purple contours are from the THOR+VGPS map at 25, 50, 150, 200, 300, and 350 mJy beam−1. The colored and black subregions are defined in the caption of Figure 9.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: A simple model of the magnetic field within an expanding SNR shell and the  B  ∥ magnetic field components along two lines of sight. The black lines represent the Galactic magnetic field. The cross-hatched region indicate the location of synchrotron emission within the SNR shell. The blue vectors represent  B  ∥ along line of sight 1. The red vectors represent  B  ∥ along line of sight 2. The lengths of the vectors do not represent the strength of  B  ∥, only the vector orientation being toward or away from the observer is represented.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: (a) The Faraday depth map (in grayscale) with WISE λ22 μm intensity (orange contours at 210, 215, and 220 W m−2 sr−1). (b) WISE λ22 μm image (in grayscale) with THOR+VGPS 21 cm continuum intensity (green contours at 20, 30, 55, 80, 110, and 140 mJy beam−1). The purple circles indicate the locations of H II regions from the WISE catalog with the size of the circle corresponding to the published size. The red + symbols correspond to stars that were identified from the WISE 3.4 μm map. The cyan “×” symbol identifies the location where Anderson et al. (2018) detected RRLs from the H II region G39.294 − 00.311 at V LSR  =  53.7 kms−1 with a beam of 150″. The SNR was found to have V LSR  =  56 ± 2 kms−1 (Lee et al. 2020).
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: The distribution of detections of polarized emission and upper limits with respect to Stokes I. ﹩{ \mathcal P }﹩ is the percentile of the maximum Stokes I surface brightness within the SNR. The red and blue curves correspond to ﹩{ \mathcal N }\,=\,{N}_{\mathrm{UL}}/{N}_{T}﹩ and ﹩{ \mathcal N }\,=\,{N}_{\mathrm{Det}}/{N}_{T}﹩, respectively, where N UL is the number of subregions with an upper limit of fractional polarization, N Det is the number of subregions where polarization is detected, and N  T  is the total number of subregions. Each of these values represents how many of each are above the corresponding ﹩{ \mathcal P }﹩. The green data points correspond to ς, which represents the standard deviation of the Faraday depths for each subregion in N Det.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: This figure identifies the location where the off-profiles were extracted to analyze the effect the noise has on the Faraday depth profiles. Each colored rectangle outlines the region where the 500 off-profiles were found. The purple crosses indicate the location of the individual field centers within the mosaic. The cyan and pink colored circles indicate the SNR and H II region, respectively.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: (a) Enlarged Faraday depth spectrum of the profile with a red border in Figure 20. (b) Results of Stokes QU fitting. The blue and red data are Stokes Q/I and U/I, respectively. The blue and red curves are the fitted model functions for single-component Burn depolarization.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: THOR and VGPS total intensity map of the SNR G39.2−0.3. The red vectors are from THOR polarization at λ21 cm rotated to λ6 cm using the observed Faraday depth, and the green vectors are from Sino-German survey. The length of the vectors is proportional to the fractional polarization observed in the associated subregion. The orange contours from the polarization map of the Sino-German survey are at levels 10, 15, 20, 25, and 30 mK.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: (a) Faraday depth distribution for all subregions with single-component Faraday rotation. This distribution has a mean Faraday depth ﹩\bar{\phi }\,=\,197\,\mathrm{rad}\,{{\rm{m}}}^{-2}﹩. (b) Faraday depth distribution for subregions where two-component Faraday rotation is observed. The values have been shifted by ﹩\bar{\phi }﹩. The purple bars represent the highest peak, and the orange bars represent the secondary peak.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Each of these functions shows the maximum value of all 500 off-positions at every Faraday depth. The colors of the functions match the colors of the rectangles shown in Figure 28 as to which SNR is nearest.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Polarization map of SNR G39.2 − 0.3. Contours are from the THOR+VGPS map at 20, 30, 55, 80, 110, and 140 mJy beam−1. The colored and black subregions are defined in the caption of Figure 9.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Illustration of the extraction of the relative mass mixing ratios ω  A  and ω  B  = 1 − ω  A  and the ratio H/R  S  for the toy example with three spectral bins and two absorbers considered in Section 5. The left panel depicts the family of vectors ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{A},{\tilde{\omega }}_{B})﹩, color coded by the value of ﹩{\tilde{\omega }}_{A}﹩. The dotted line marks the direction of ﹩{\overrightarrow{r}}_{\perp }﹩ defined by (46). The right panel shows the relationship between the trial value ﹩{\tilde{\omega }}_{A}﹩ and the resulting direction of ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{A},{\tilde{\omega }}_{B})﹩ in terms of its polar angle φ (in units of π).
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: A ternary plot illustrating the retrieval of the relative mass mixing ratios ω  A , ω  B , and ω  C  for the example discussed in Section 6. Each point on the plot represents a unique combination of the trial values ﹩{\tilde{\omega }}_{A}﹩, ﹩{\tilde{\omega }}_{B}﹩, and ﹩{\tilde{\omega }}_{C}﹩, subject to ﹩{\tilde{\omega }}_{A}+{\tilde{\omega }}_{B}+{\tilde{\omega }}_{C}=1﹩, with a scan resolution of ﹩{\rm{\Delta }}\,\tilde{\omega }=0.005﹩. The points are color coded by the value of the relative angle ΔΘ (in radians) between the fixed measured vector ﹩{\overrightarrow{r}}_{\perp }﹩ and the trial vector ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{A},{\tilde{\omega }}_{B},{\tilde{\omega }}_{C})﹩. The white cross marks the true values of ω  A , ω  B , and ω  C .
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Results for the underconstrained example discussed in Section 7. The left panel shows the trial family of vectors ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{a})﹩ (scanned with resolution ﹩{\rm{\Delta }}\tilde{\omega }=0.002﹩), in complete analogy to the left panel of Figure 1 and the right panel of Figure 2. Here the transverse space is two-dimensional (as in Figure 1) and the locus of points representing ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{a})﹩ is two-dimensional as well (as in Figure 2). The measured direction of ﹩{\overrightarrow{r}}_{\perp }﹩ indicated by the black dotted line is in the plane of the figure, and the ⋆ symbol marks the true value of ﹩{\overrightarrow{L}}_{\perp }.﹩ The right panel shows the corresponding ternary plot illustrating the results from the retrieval for this case, in analogy to Figure 3.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: The same as the left panel in Figure 1, but for the example discussed in Section 6. The three-dimensional family of transverse vectors (57) is color coded by the trial value ﹩{\tilde{\omega }}_{B}﹩ (left panel) or ﹩{\tilde{\omega }}_{C}﹩ (right panel). The dotted line emerging from the origin O of the coordinate system shows the measured direction of ﹩{\overrightarrow{r}}_{\perp }﹩ according to (55).
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: These figures display the distribution of fractional polarization and Faraday depth for the Faraday profiles extracted from the H II regions shown in Figure 28. The red and yellow distributions correspond to the H II regions near SNRs G46.8 − 0.3 and G43.3 − 0.2, respectively. The green and blue distributions correspond to the H II regions near SNRs G41.1 − 0.3 and G39.2 − 0.3, respectively. Columns (a) and (c) show the distribution of fractional polarization, which was found using the same method as for the SNRs (see Figure 9). Columns (b) and (d) show the distribution of Faraday depth.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Representation of the degenerate solutions found in the retrieval analysis of Section 7. All points from the ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{a})﹩ grid with ΔΘ < 0.001 are plotted in the ﹩({\tilde{\omega }}_{B},{\tilde{\omega }}_{C})﹩ plane and color coded by the value of ﹩{\tilde{\omega }}_{A}﹩ (left panel) or the ratio of ratios (59) (right panel).
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Wavelength dependence of the dimensionless absorption coefficients ξ  a  defined in (19) for water (left panel) and HCN (right panel). Each panel shows results for 10 different values of the temperature, starting from T = 500 K and increasing by ΔT = 250 K.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: The transit spectrum for the study point (60c) analyzed in Section 8.
Paper: The Velocity Dispersion Function for Massive Quiescent and Star-forming Galaxies at 0.6 < z ≤ 1.0
Authors: Lance Taylor, Rachel Bezanson, Arjen van der Wel, Alan Pearl, Eric F. Bell, Francesco D'Eugenio, Marijn Franx, Michael V. Maseda, Adam Muzzin, David Sobral, Caroline Straatman, Katherine E. Whitaker, Po-Feng Wu, 柏鋒 吳
Figure caption: Our measurements of the VDF in the context of previous literature measurements in the local universe (top row) and at higher redshifts (bottom row) and split into quiescent (left) and star-forming (right) populations. Previous measurements vary significantly in sample selection and methodology, including reliance on several indirect measurements of velocity dispersions. This work (colored bands) represents the first direct measurement of the VDF for the full population of galaxies beyond the local universe, collapsing previous systematic uncertainties in our understanding of the evolving distribution of gravitational potential wells.
Paper: The Velocity Dispersion Function for Massive Quiescent and Star-forming Galaxies at 0.6 < z ≤ 1.0
Authors: Lance Taylor, Rachel Bezanson, Arjen van der Wel, Alan Pearl, Eric F. Bell, Francesco D'Eugenio, Marijn Franx, Michael V. Maseda, Adam Muzzin, David Sobral, Caroline Straatman, Katherine E. Whitaker, Po-Feng Wu, 柏鋒 吳
Figure caption: VDFs of quiescent (red), star-forming (blue), and all galaxies (purple) for 0.6 < z ≤ 1.0 (left panel) and in bins of Δz = 0.1 (center and right panels). The points (left panel) and lines (center and right panels) are the VDFs calculated using the direct spectroscopic measurements from LEGA-C. The red, blue, and purple bands are 1σ ranges for the best-fit modified Schechter function. The gray band (center) and black line (right) are the most recent z ≃ 0 VDFs from the literature for each respective population (quiescent: Sohn et al. 2017; star-forming: Bernardi et al. 2010). Both galaxy populations exhibit remarkable stability in Φ(σ ⋆,vir) from z ∼ 1 until today, although there appears to be weak evolution of number densities for star-forming galaxies within the redshift range probed by LEGA-C.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Ternary plots analogous to Figure 3, which illustrate the extraction of the weights ω  A , ω  B , and ω  C . Each panel corresponds to a different a priori trial guess ﹩\tilde{T}﹩ for the atmospheric temperature, as indicated in the titles. The input temperature for this example was T = 2000 K. The points are color coded by the value of the relative angle ΔΘ (in radians) between the fixed measured vector ﹩{\overrightarrow{r}}_{\perp }﹩ and the corresponding trial vector ﹩{\overrightarrow{L}}_{\perp }({\tilde{\omega }}_{A},{\tilde{\omega }}_{B},{\tilde{\omega }}_{C},\tilde{T})﹩ from (62). As before, the white cross marks the true values of ω  A  = 0.342, ω  B  = 0.513, and ω  C  = 0.144.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Results from 10,000 pseudoexperiments performing the transverse vector decomposition retrieval method on the nominal spectrum from Figure 7 with added Gaussian noise at the level of 10 ppm, 30 ppm, or 50 ppm. In each pseudoexperiment we retrieve the values of ω  A  (top row), ω  B  (second row), ω  C  (third row), and H/R  S  (bottom row). The histograms in the left column show distributions of the retrieved values of the parameters for noise levels of 10 ppm (orange histograms) and 30 ppm (blue histograms), while the right column shows the corresponding box and whiskers plots illustrating the accuracy of the retrievals. The black dashed lines mark the true values of the parameters.
Paper: Transverse Vector Decomposition Method for Analytical Inversion of Exoplanet Transit Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: The quality of the retrieval procedure as a function of the assumed trial temperature ﹩\tilde{T}﹩. The left panel shows the minimum angle ΔΘ found in the fit with a scan resolution of ﹩{\rm{\Delta }}\,\tilde{\omega }=0.002﹩. An ideal fit with ﹩{\rm{\Delta }}{{\rm{\Theta }}}_{\min }=0﹩ is achieved for the true value of the temperature T = 2000 K. The right panel shows the corresponding retrieved value of R  S /H from (38), where the horizontal red dashed line denotes the true value R  S /H = 1542.
Paper: The Velocity Dispersion Function for Massive Quiescent and Star-forming Galaxies at 0.6 < z ≤ 1.0
Authors: Lance Taylor, Rachel Bezanson, Arjen van der Wel, Alan Pearl, Eric F. Bell, Francesco D'Eugenio, Marijn Franx, Michael V. Maseda, Adam Muzzin, David Sobral, Caroline Straatman, Katherine E. Whitaker, Po-Feng Wu, 柏鋒 吳
Figure caption: The fraction of quiescent galaxies as a function of log σ ⋆,vir. The quiescent fraction for the full redshift range of LEGA-C (0.6 < z ≤ 1.0) is shown as a gray band. Points with error bars show the function in bins of Δz = 0.1. The 50% threshold between quiescent or star-forming dominance is designated by the dashed line. Quiescent galaxies dominate at high-velocity dispersions, while star-forming galaxies are more common at low sigmas. The crossover threshold of ∼170 km s−1 may evolve slightly (∼10%) within the LEGA-C redshift range.