adsabs/AstroCLIMB huggingface dataset:
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Atmospheric buildup of CH3Br in planetary atmospheres around different stellar types for a variety of surface flux conditions based on those seen on the Earth. Compare to Figure 4. Mixing ratios in the green region are comparable to Earth’s preindustrial methane abundance.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Size–linewidth–surface density plots, adapted from O’Neill et al. (2022) with the addition of N90 clumps. (a) Velocity dispersion σ  v  compared to radius R of clumps from studies described in Section 4.1. The arrows show the corrections needed to account for CO-dark gas on observable CO clump properties for a typical clump with [R CO = 0.40 pc, M(R CO) = 13 M ⊙, σ  v (R CO) = 0.45 km s−1]. The arrows move from the properties of the observed CO clump to the inferred full state of the clump including CO-dark gas. The dark blue arrow follows a velocity profile σ  v  ∝ R 0.5 [β = 0.5], and the light blue arrow follows a velocity profile σ  v  ∝ R 0.25 [β = 0.25]. Both arrows show the effect for a density profile ρ ∝ R −1 [k = 1] and f DG ∼ 0.8. The gray dashed line follows the relationship σ  v  = 0.72R 0.5 derived by SRBY, and the gray dotted line is the expected σ  v  at T = 20 K from thermal motion. The black solid line was fit to the N90 clumps and follows σ  v  = 0.98 R 0.81. (b) Size–linewidth parameter ﹩{\sigma }_{v}^{2}/R﹩ compared to surface density Σ, with correction arrows as in (a). The black line corresponds to virial equilibrium (Equation (9) with k = 0), and the black curves correspond to virial equilibrium under varying degrees of external pressure (with units of P/k in K cm−3, Equation (11) with Π = 0.6).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Spatial variation of CO clump characteristics, with the HST Hα image shown in gray. (a) The regions we define as part of the rim are shown in green, and the corresponding nonrim regions are marked in blue. The 2D clump boundaries identified by the quickclump algorithm are shown in white. Details of the two orange rectangles A and B are shown in Figure 6. (b) Average surface density Σ of clumps, with point sizes proportional to clump area. (c) Maximum clump excitation temperature T ex. (d) Peak 12CO velocity of clumps, with the red/blue color scale centered at the mean radial velocity (RV) of H I components surrounding N90, vLSRK ∼ 170 km s−1, as derived from Fukui et al. (2020) and Nigra et al. (2008).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Star formation efficiency (SFE) ϵ′ = SFR/M cloud is compared to cloud mass M cloud. The ϵ′ value we derived from the CO-bright gas mass in N90 using an X CO,B  conversion factor (X CO,B  = 3.4 × 1020 cm−2 (K km s−1)−1) is shown along with the ϵ’ derived through correcting for CO-dark gas mass (f DG ≃ 0.8; Section 4.2) by the labeled blue points. The ﹩\epsilon ^{\prime} ﹩ we derived for SGS 1 is marked with a black diamond. Results for a sample of LMC GMCs analyzed by Ochsendorf et al. (2017) are shown: pink squares had masses derived through α CO conversion, and purple diamonds had masses derived from Jameson et al.’s (2016) dust-based molecular hydrogen map of the LMC. A sample of Galactic clouds studied by Lee et al. (2016) is also shown by gray circles.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Top: expanded image of Figure 7(a)’s Region A, along the west rim near the massive star Sk 183 (labeled). Contours of integrated 12CO intensity are shown, with levels of 0.25, 0.5, 0.75, and 1 Jy beam−1 km s−1 drawn in yellow, green, teal, and blue, respectively. The synthesized beam size for the CO observations is shown in the lower-left corner. The locations of YSO candidates are shown by red stars. The HST ACS Hα image is shown in gray. Bottom: the same as in the left panel, but for Figure 7(a)’s Region B, on the east rim near NGC 602 (labeled).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Kernel density estimations (KDEs) comparing physical properties of clumps on the N90 rim (red) and not on the N90 rim (blue), with both groups assigned as in Figure 7(a). p-values resulting from two-sided K-S tests comparing the rim vs. nonrim distributions are shown in each panel, with any p < 0.05 set in bold to indicate that there is a statistically significant difference between the distributions. Top: excitation temperature T ex. Second from top: velocity dispersion σ  v . Third from the top: radius R. Bottom: surface density Σ.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Clump virial mass M vir is compared to clump X CO,B -derived mass ﹩{M}_{{X}_{\mathrm{CO},B}}﹩. The black dashed line shows a 1:1 relationship where ﹩{M}_{\mathrm{vir}}={M}_{{X}_{\mathrm{CO},B}}﹩, i.e., where the virial parameter α vir = 1 and stability could be expected, and the blue line shows a best-fit relationship M vir/﹩{M}_{{X}_{\mathrm{CO},B}}﹩ = 19 ﹩{M}_{{X}_{\mathrm{CO},B}}^{-0.34}﹩. The two mass distributions are represented individually by Gaussian KDEs placed horizontally on the top axis of the scatter plot (﹩{M}_{{X}_{\mathrm{CO},B}}﹩) and vertically on its left axis (M vir).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Locations of stars in F555W—F814W, F814W color–magnitude space. PMS stars are marked with dark gray triangles, and non-PMS stars are marked with light gray squares. PMS isochrone models for ages between 0.5 and 6 Myr are shown as colored curves. A reddening vector for A  V  = 0.25 mag is shown by the thick black solid arrow, and for A  V  = 1.6 mag by the thin black dashed arrow.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Locations of the PMS star clusters identified by the DBSCAN algorithm. PMS stars are marked with triangles. The clusters are denoted by color, and are labeled with their Table 1 ID numbers and the mean ages of their members. Nonclustered PMS stars are marked with gray triangles. The Hα image is in gray, and contours of integrated 12CO(2–1) emission at 0.25 Jy beam−1 (km s−1)−1 are shown in green.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Top: the virial parameter α vir is compared to projected distance to NGC 602 for clumps in the eastern half of N90. The value of Spearman’s ρ  s  rank correlation coefficient for the two variables is shown in the top right. Bottom: the same as the top, but for projected distance to the massive star Sk 183 for clumps on the western half of N90.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: The HST ACS Hα image is shown with the locations of PMS stars (yellow points), YSO candidates (red triangles), and the 2D boundaries of the CO clumps identified by the quickclump algorithm (light blue contours).
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Properties of the massive quiescent galaxies in the z ≳ 3 sample that have published stellar velocity dispersions. Left: the rest-frame color UVJ diagram. Galaxies are labeled here and in subsequent plots by the reference containing stellar velocity dispersion measurements. Rest-frame colors, star formation rates, and/or stellar masses are often from separate publications, also noted. Data at z ≳ 3 are shown as a gold upward-facing triangle (Tanaka et al. 2019), a seagreen downward-facing triangle (Saracco et al. 2020), azure squares (Esdaile et al. 2021), and raspberry circles (this work). Right:  the relation between the star formation rate and stellar mass. Galaxies with photometric redshifts 3 < z < 4 from the COSMOS-UltraVISTA DR3 catalog are shown as black points, and dashed lines are plotted showing a constant specific SFR (−1.5 and −0.5 Gyr−1), corresponding roughly to the main sequence and 1 dex below it.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Ratio of dynamical-to-stellar mass (IMF mismatch parameter) plotted against velocity dispersion at the half-light radius. The best fit to the data from Posacki et al. (2015) at z ∼ 0.2 is shown in purple, while the best fit to the data from Mendel et al. (2020) at 1.4 < z < 2.1 is shown in gray. Data at z > 3 are shown in the same colors as the previous plot, while the fit is in turquoise. Average error ellipses for the data sets from Posacki et al. (2015), Mendel et al. (2020), Esdaile et al. (2021), and this work are shown in the bottom right. Horizontal dashed lines show the result when using a Salpeter or Chabrier IMF, below which using the respective IMF results in a stellar mass greater than the dynamical mass.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Effective radii and stellar masses of the massive galaxies. Colors and markers remain the same as in Figure 4, and objects with sizes derived from high-resolution HST imaging have white centers. Representative error bars for the Mendel et al. (2020) data set are shown on the left. The three galaxies with SFR > 3 M ⊙ yr−1 are marked with a black star and excluded from the z ≳ 3 fit. The size–mass relations for early-type galaxies at z ∼ 0.25 and z ∼ 1.75 from van der Wel et al. (2014) are shown as purple dashed lines, while fits to the Mendel et al. (2020) data set and the z ≳ 3 data set are a black line and a solid turquoise line with the range of Monte Carlo fits from 16%–84% shaded accordingly.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Stellar velocity dispersions and stellar masses of the massive quiescent galaxies. The colors and markers used for the z ≳ 3 sample are identical to those in Figure 3, while data from Mendel et al. (2020) at 1.4 < z < 2.1 are shown in gray. The median error bar for the Mendel et al. (2020) data set is ∼0.1 dex. Fits to both sets of data are shown as turquoise and gray lines, respectively, with shaded error regions representing the 16th to 84th percentile range from Monte Carlo resampling. The fit to low-redshift data from Zahid et al. (2016) is shown in purple.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Similar to Figures 5 and 7, with additional low-redshift, high velocity dispersion ETGs (green circles; Bernardi et al. 2006). The arrows on the size–stellar mass relation (left) show the effect on those properties via various merger scenarios, normalized to a doubling of the stellar mass.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Effective radii for the UMGs. Radii measured directly from the K band and F160W imaging are shown as squares colored red and blue, respectively. Correcting these sizes to 5000 Å radius results in circles of the same colors. The weighted average of the corrected measurements (the same as the K-band value if F160W data are unavailable) is shown as a black triangle. The pixel size of the imager at the redshift of each target is shown as a black line, while the FWHM/2 is a gray dashed line.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: The observed H- and K-band spectra for the MAGAZ3NE UMGs (black) and associated error spectra (gray). The best-fit pPXF model is shown in red. The wavelengths of prominent features from oxygen (magenta), calcium (green), and hydrogen (gold) are indicated as vertical dashed lines. When emission lines are present, we mask these features in the velocity dispersion fit.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Dynamical and stellar masses of the massive quiescent galaxies. The colors and markers used are identical to those in Figure 5. The black dashed line represents a ratio of unity, corresponding to a Chabrier IMF.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top-left panel shows the T(P) profile of brown dwarf models with log(g) = 5 and T eff of 500, 700, and 1000 K. The solid T(P) profiles assume disequilibrium chemistry self-consistently whereas the dotted profiles show equilibrium chemistry calculations. The convective zones are shown with thicker lines for each T(P) profile. To differentiate the convective zones of the equilibrium chemistry models from the disequilibrium chemistry models, they are shown with much thicker lines compared to the convective zones of disequilibrium chemistry models. The top-right panel shows the plotted CO volume mixing ratio profiles for these brown dwarf models. The solid lines show the mixing ratio with disequilibrium chemistry whereas the dotted lines show calculations from equilibrium chemistry. The bottom panel shows the normalized thermal emission spectra of these brown dwarfs. The solid lines show the disequilibrium chemistry results, while the dotted spectra represent the equilibrium chemistry calculations. The J, H, K’, L’, and M’ bands are also shown as shaded regions of different colors. The main point here is that self-consistent treatment of disequilibrium chemistry leads to large changes in the T(P) profile, abundances, and thermal emission spectra.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top panels show the τ = 1 pressure levels for specific gaseous absorbers in a model T-dwarf with T eff = 700 K and log(g) = 5.0 in the presence and absence of quenching due to vertical mixing. τ = 1 pressure levels for H2O, CH4, CO, and NH3 are shown in the first, second, third, and fourth columns, respectively. The equilibrium chemistry pressure levels are shown by the dashed lines, whereas the disequilibrium chemistry pressure levels are shown by the solid lines. The volume mixing ratio as a function of the pressure of each gas in the presence (solid lines) and absence (dashed lines) of vertical-mixing-induced quenching are also shown by the black lines in the top x-axis of each of the top four panels. The bottom panel shows the logarithm of the pressure ratio of these τ = 1 levels with equilibrium chemistry and disequilibrium chemistry for the gaseous absorbers. The zero mark represents no change in these pressure levels. Positive values represents an increase in absorption in the disequilibrium chemistry models compared to equilibrium chemistry models. The main point here is that disequilibrium chemistry leads to large opacity changes in the atmosphere.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: The reduced χ 2 for COS-DR3-84674 compared to velocity dispersion for BC03 templates demonstrating the age–metallicity degeneracy. The χ 2 values are taken from the FAST++ joint fit to both photometric and spectroscopic data and are normalized to the lowest value by scaling the input spectral errors. The 1σ and 2σ significance given the number of degrees of freedom are indicated by horizontal lines. Each colored line represents templates with a set metallicity, while each point is a different age template.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Velocity dispersion fit as a result of trimming the observed spectra. Blue lines represent the velocity dispersion returned when the spectrum is fit from the rest-frame wavelength on the abscissa to the reddest wavelength available. Red lines represent the velocity dispersion returned when the spectrum is fit from the bluest wavelength available to the wavelength on the abscissa. Shaded regions show the uncertainties returned by pPXF for each measurement. An additive polynomial of order d = 10 is used for this example.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Velocity dispersion dependence upon choice of additive polynomial order for COS-DR3-84674. Results are calculated for 0 ≤ d ≤ 50, with the gray shaded region indicating the uncertainties returned by pPXF for each measurement. The red dashed line indicates the median value across all choices of d, the shading between the 16th and 84th percentiles. The blue dashed line is the median value over 5 ≤ d ≤ 20.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: The distribution of measured velocity dispersions returned by pPXF for each of the MAGAZ3NE objects presented in this work. Here, each run of pPXF is convolved with a Gaussian kernel with a width equivalent to the uncertainty reported by pPXF and additionally weighted by the reduced χ 2 of the fit. The weighted average is also labeled. This is the value transformed to σ e by performing an aperture correction.
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Velocity dispersion fit as a result of choice of template library with all other parameters fixed. Templates from the MILES library (light gray triangles), Indo-US library (dark gray squares), and Bruzual & Charlot models (black circles) are shown for each galaxy.