adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Histograms of the ratios among CO, Hα, and mid-IR emission. Histograms showing log10 ratios of (top two rows) CO to mid-IR emission, (middle rows) extinction-corrected Hα to mid-IR emission, and (bottom row) CO to extinction-corrected Hα. The lines and shaded regions show the median and 16%–84% range reported in the main text of the paper (Table 4 and Figure 14). Note that we show only values with a positive ratio, but this caveat affects only a small subset of the CO data (e.g., see that the 16% to 84% range is positive).
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: Panel (a): [C II] line spectrum from the 30 km s−1 ALMA data cube (Fujimoto et al. 2022b). Panel (b): False-color RGB JWST/NIRCam image zoomed in on S04590 (blue: F150W; green: F277W; red: F444W), overlaid with the 2σ, 3σ, and 4σ contours of the [C II] moment-0 map with the beam size represented by the white ellipse. Panel (c): JWST/NIRSpec spectrum with the most prominent nebular and auroral emission lines marked. Panel (d): Best-fit SED model (black curve) and model photometry (red points) based on the derived JWST/NIRCam+NIRISS photometry (blue points) using BAGPIPES (Carnall et al. 2018) and assuming the dust attenuation curve from Salim et al. (2018).
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: (Top panel) Total gas mass excess, M gas/M ⋆, as a function of redshift. For the local galaxy sample at z ∼ 0 (Leroy et al. 2008), ﹩{M}_{\mathrm{gas}}={M}_{\mathrm{HI}}+{M}_{{{\rm{H}}}_{2}}﹩. For the high-z galaxy sample compilation (see main text for references), we assume that the total gas mass can be estimated as M gas = M dyn,tot − M ⋆, with M dyn,tot estimated from the [C II] line width and spatial extent. Gray boxes indicate the redshift distributions and standard deviations for each sample. Overall, M gas/M ⋆ increases with redshift by a factor of ≈10 from z ∼ 0 to z ∼ 7, and ﹩\mathrm{log}({M}_{\mathrm{gas}}/{M}_{\star })=0.9\mbox{--}1.7﹩ for S04590. (Bottom panel) Total gas depletion time, t depl = M gas/SFR, as a function of redshift; t depl is observed to decrease by a factor of ≈10 on average from z ∼ 0 to z ∼ 7.
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: Gas mass fraction, f gas = M gas/(M gas + M ⋆), as a function of stellar mass. The symbol notation follows Figure 3. We observe an overall anticorrelation of f gas with stellar mass for both the low- and high-z galaxy samples, though with an offset due to the redshift evolution of M gas/M ⋆. S04590 and I Zw 18 are both clear outliers, with low stellar masses M ⋆ = 1–2 × 107 M ⊙ and high gas fractions f gas ≳ 90%, but seem to follow the overall trend.
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: DTG (top) and DTM (bottom) mass ratios as a function of the gas-phase metallicity, ﹩12+\mathrm{log}﹩(O/H). The red and gray star symbols highlight S04590 and I Zw 18, respectively. The gray dots represent the local z ≈ 0 DUSTPEDIA galaxy sample from De Vis et al. (2019), with their best-fit DTG–metallicity relation shown by the dashed line. The colored filled circles show line-of-sight measurements through quasar absorbers at z ≈ 1–4 (Péroux & Howk 2020), color-coded as a function of redshift. Both S04590 and I Zw 18 are among the most dust-poor galaxies known, but are consistent with the overall evolution with metallicity.
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: MZ relation of S04590. For comparison, we show the various preexisting MZ estimates for S04590 from the literature, which highlights the uncertainties from the various methods used. We also show various MZ relations either observed for galaxies at z ≈ 0 and z ≈ 3.3 (black and green, respectively; Sanders et al. 2021) and at z ≈ 7–10 (Heintz et al. 2022b) or predicted from the Astraeus (Ucci et al. 2023) and FIRE (Ma et al. 2016) simulations, extrapolated to z ≈ 8. The local, metal-poor galaxy I Zw 18 is marked by a gray star symbol, showing an MZ relation consistent with that of S04590. Both are consistent with the predictions for high-z MZ relations.
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: Zoomed-in views of the regions of the spectrum that include the main nebular and auroral emission line transitions examined in this work. The black line shows the flux density, with the gray region represents the noise level. The best-fit continuum and Gaussian profiles to each line transition are shown by the dashed red line. The [O II] λλ3726, 3728 doublet is not resolved at this spectral resolution.
Paper: The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA
Authors: K. E. Heintz, C. Giménez-Arteaga, S. Fujimoto, G. Brammer, D. Espada, S. Gillman, J. González-López, T. R. Greve, Y. Harikane, B. Hatsukade, K. K. Knudsen, A. M. Koekemoer, K. Kohno, V. Kokorev, M. M. Lee, G. E. Magdis, E. J. Nelson, F. Rizzo, R. L. Sanders, D. Schaerer, A. E. Shapley, V. B. Strait, S. Toft, F. Valentino, A. van der Wel, A. P. Vijayan, D. Watson, F. E. Bauer, C. R. Christiansen, S. N. Wilson
Figure caption: Cornerplot of SED posterior distributions from BAGPIPES.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Comparison among intensities in different mid-IR bands at matched resolution in the first four PHANGS–JWST target galaxies. Each panel compares a different mid-IR band and F770W. For pairs of JWST MIRI bands, the pink points and red bins show the comparison at the θ = 1.″7 resolution used in the main text of this paper. For all bands, the blue points and bins show comparisons after convolution of all data to a common Gaussian beam with FWHM θ = 15″. The bins show the median and 16%–84% range for the y-axis band when binned by F770W intensity quantity. The dashed black lines show linear fits to the bins for the 15″ data, which also describe the 1.″7 data well. The fits appear overall consistent with passing through the origin, indicating a self-consistent overall background level among all data and good agreement with previous mapping that covered wider areas at coarser resolution. The slopes of these lines are the fiducial band ratios that we adopt in the main text (Table 1), and the scatter in the blue points sets the reported scatter in that table. The scatter among the best-fitting intercepts informs our estimate that the JWST MIRI background levels are currently uncertain by ∼±0.1 MJy sr−1. The overall consistency and linearity motivate our suggested approach to background level adjustment or validation in Appendix B.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Best-fitting power-law slopes comparing mid-IR, CO (2–1), and extinction-corrected Hα. Each point shows the slope, m, from Equations (10) and (11), for one variable pair and data set. Colored points show results from fitting our full combined data set. Overall, the figure shows consistent results for individual galaxies and the combined data set, with the lower-mass, lower-metallicity IC 5332 the most consistent outlier. The CO vs. mid-IR relation shows slopes fairly close to unity (the black line), corresponding to a linear relation. Meanwhile, the extinction-corrected Hα shows a consistently steeper slope vs. mid-IR, indicating high Hα-to-mid-IR ratio in bright star-forming regions. CO (2–1) vs. extinction-corrected Hα shows a much shallower slope when treating Hα as the independent variable, consistent with approaching the scale where the CO–Hα correlation breaks down. Throughout, F2100W shows a moderately different behavior from the other three mid-IR bands (Section 4.4). See Table 4 for the corresponding numerical results and Section 4 for discussion.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Summary CO-to-mid-IR and extinction-corrected Hα-to-mid-IR median ratios and template-matching coefficients. Each point in the left panel shows a CO (2–1) to mid-IR ratio, and each point in the right panel shows an extinction-corrected Hα-to-mid-IR ratio. To allow easy comparisons between bands, all ratios have been scaled to an F770W intensity scale using the coefficients in Table 1. The blue and red points with error bars show the median ratios and scatter from Table 4. The green and purple points show results from the model-fitting analysis in Table 5. Gray points show results for individual galaxies. The solid black lines show conversions based on the equations in Section 2 that describe the template-fitting coefficients reasonably well. For the CO, this is emission from a Draine & Li (2007) model with D/G = 0.01 and an ISRF U/U 0 = 2.5. For the Hα, this is an SFR conversion with normalization C 24 = 10−42.9. The ratios show consistently lower ratios than the templates, reflecting that both heating and column density terms contribute to the overall distribution.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR intensity predicted from a linear combination of CO and extinction-corrected Hα as a function of observed mid-IR intensity. As Figures 5 and 7 but now showing our model constructed from a linear combination of scaled I CO and I Hα  (Equation (12), Section 5) as a function of the observed mid-IR intensity. We use the best-fitting coefficients for each individual galaxy (Table 5 and the points in Figure 11) and color the data by the mean fractional contribution of the Hα component in that bin. That is, in yellow bins, the model assigns more flux to the Hα-tracing component while in dark green regions, the CO-tracing component contributes most of the flux. The red lines show equality. The shaded regions show the limits of our definition of “bright” emission, which represents the extent of the data fit. See Figure 13 for individual galaxy fits.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Template-matching model goodness of fit vs. CO and Hα scaling coefficients, c and h. Mean absolute log residual for models that attempt to match observed bright mid-IR emission with a linear combination of scaled CO and scaled Hα emission (Equation (12); Section 5). The contours and color image show goodness of fit using all data as a function of possible ﹩{\mathrm{log}}_{10}c﹩ and ﹩{\mathrm{log}}_{10}h﹩. All four bands yield a clear minimum, shown by the circle, at physically plausible values (Section 6), which imply roughly equal flux associated with the CO-tracking and Hα-tracking components. We run a similar minimization for each target galaxy independently, and the figure shows the resulting best-fitting coefficients for each galaxy. The variations from galaxy to galaxy appear similar from band to band, and we expect these reflect real physical variations, e.g., in the ISRF, dust-to-gas ratio, and level of extinction, among our targets. Table 5 gives fits for all bands and targets. Figures 12 and 13 show the model vs. observation for these fits.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Extinction-corrected Hα intensity as a function of mid-IR intensity at 1.″7 resolution, separated by galaxy. As Figure 7 but now showing the binned relation between extinction-corrected Hα and mid-IR intensity for each individual galaxy and band (colored points) along with a power-law fit to the binned data for each galaxy (colored lines). The dark gray-shaded curve represents the 16%–84% range for the full data set and the gray line indicates the best-fitting power law for all data seen as a red line in Figure 7. The figure legends list the slope (m) for each fit. See Table 4 for the full numerical fit values.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR intensity predicted from a linear combination of CO and extinction-corrected Hα as a function of observed mid-IR intensity, separated by galaxy. As Figures 6, 8, and 9 but now showing the mid-IR intensity predicted by our model (Equation (12), Section 5) as a function of observed mid-IR intensity for individual galaxies. As in those figures, the dark gray region shows results for all galaxies combined with the extent showing the 16th to 84th range. The individual symbols show median results for individual galaxies and the line indicates one-to-one agreement. Overall, the agreement between prediction and observation appears excellent for all four galaxies, with the models failure to account for suppression of PAH emission in H II regions leading to mild overpredictions at high F770W, F1000W, and F1130W intensities.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: CO (2–1) intensity as a function of extinction-corrected Hα intensity. The left panel follows Figures 5 and 7 but now plotting CO (2–1) intensity as a function of extinction-corrected Hα intensity color-coded by 10 μm intensity. The right panel similarly follows Figures 6 and 8, showing results for individual galaxies. Annotations follow the other figures: shading shows regions excluded from statistical analysis, the thick red (left) and black (right) lines show the best-fitting power law to the binned data for all galaxies, and colored lines show power-law fits for individual galaxies, with m and b giving the slope and intercept of the fits respectively.