adsabs/AstroCLIMB huggingface dataset:
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Comparison between the observed C18O radial profiles (Law et al. 2021; gray) and simulated observations. A model without drift is shown in black. Colored lines show models with an increased surface density in the inner disk due to drift. The 540 M ⊕ model is the 1 mm drift model shown in Figure 1; the others are the same model scaled up or down a factor of 2 in surface density. An inner-disk mass of more than 540 M ⊕ within 20 au is required to have an inner-disk depression.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Histogram of η  γ  from 10,000 MC samplings; each bin corresponds to the η  γ  interval of 0.003. The histogram is fitted by a skew-normal distribution function.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Same as Figure 2 but for 13CO instead of C18O. Again, >540 M ⊕ is required to create an inner-disk depression.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Schematic of the dust (orange) and gas (blue) distributions in the IM Lup disk. A planet image has been put in the approximate position of a proposed protoplanet around 100 au (Pinte et al. 2020; Verrios et al. 2022).
Paper: PHANGS–JWST First Results: Destruction of the PAH Molecules in H II Regions Probed by JWST and MUSE
Authors: Oleg V. Egorov, Kathryn Kreckel, Karin M. Sandstrom, Adam K. Leroy, Simon C. O. Glover, Brent Groves, J. M. Diederik Kruijssen, Ashley. T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Eric Emsellem, Kathryn Grasha, Ralf S. Klessen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Erik Rosolowsky, Fabian Scheuermann, Eva Schinnerer, Jessica Sutter, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: Correlation of PAH abundance, traced by R PAH, with ionization parameter, traced by log([S III]/[S II]) (panels (a) and (b)) or ionization fraction f ion (panels (c) and (d)). Color encodes the oxygen abundance ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ (panel (a)); ratio of F1130W/F770W, a proxy for the ionization state of PAHs (panel (b)); number of hydrogen-ionizing photons Q 0 (panel (c)); and effective radii of the H II regions relative to the PSF of the MUSE data (panel (d)). Dashed lines show a linear fit for the H II regions (Equation (2) for panels (a) and (b)). Faint (Q 0 < 1050 s−1;  green dashed line, Equation (3)) and bright (Q 0 > 1050 s−1;  magenta dashed line, Equation (4)) H II regions are considered separately in panels (c) and (d). Spearman’s correlation coefficient (ρ) is given in the corner of each plot. Coefficients ρ 1 and ρ 2 are calculated separately for the black and cyan points (panels (b) and (d)) or faint and bright regions (panel (c)), respectively. The errors on ρ are derived from 1000 Monte Carlo realizations with the data randomly distributed around the measured values within the uncertainties.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Disk-averaged CO-to-mid IR intensity ratio as a function of galaxy specific star formation rate. As Figure 9 but now comparing I CO/I MIR to SFR/M ⋆. We caution that because of the use of 22 μm emission as part of the SFR estimate the axes are internally anticorrelated. Nonetheless, the observed anticorrelation between I CO/I MIR to SFR/M ⋆ matches recent results that link the molecular gas depletion time to offsets from the main sequence (Saintonge et al. 2016; Colombo et al. 2018, 2020). The steeper slope for 22 μm compared to 12 μm emission could reflect a dependence of PAH abundance on SFR/M ⋆, also broadly consistent with recent observations.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Disk-averaged CO-to-mid-IR intensity ratio as a function of galaxy stellar mass. Each point shows a measurement for an integrated galaxy, with galaxies that have a resolved CO map suitable for comparison to the mid-IR (i.e., relatively nearby galaxies with large angular sizes of several arcminutes) marked with black star symbols. The bins show an overall weak correlation of the CO-to-mid-IR ratio with stellar mass. This could be indicative of a combination of atomic gas and CO-dark molecular gas contributing some mid-IR emission in low-mass galaxies, or alternatively comparatively brighter CO emission per molecular mass in high-mass galaxies, or perhaps a lower star formation efficiency per unit molecular gas mass at high stellar masses. The set of very nearby galaxies with large CO (1–0) maps shows significant bias relative to the overall galaxy population sampled by the integrated measurements, very likely reflecting a sample bias since these surveys were optimized to provide high-S/N detections.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: First four PHANGS–JWST target galaxies compared to our larger sample in I CO–I MIR space. As Figure 12, but now each panel shows results from the first four PHANGS–JWST targets in blue and purple. Each panel shows results for a different filter, the blue points show binned versions of the PHANGS–JWST data, and the purple lines shows fits to these binned data. For comparison, we also plot individual region results for our larger data set in the background of each panel, and show the fit to those data in black. We compare F770W, F1000W, and F1130W to the 8 μm band and F2100W to the 24 μm band. Given the small sample of four current targets, the agreement in between the PHANGS–JWST fits and those for our larger sample (Table 4) appears excellent. The F770W and F1130W results closely match those for 8 μm, while the F1000W fit shows a similar slope offset to indicate the fainter F1000W. F2100W and 24 μm also show good agreement.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Statistical inference of the CO (2–1) to CO (1–0) ratio as a function of mid-IR intensity. Inferred dependence of the CO (2–1) to CO (1–0) line ratio, R 21, on mid-IR intensity at different bands using our full data set and assuming all surveys sample the same underlying galaxy population (Equation (7)). The noise and shading are added to allow one to more easily distinguish the lines by eye, and we manually cap R 21 at 1, which we also recommend when implementing Equation (7). The statistical corrections to the local CO (1–0) mapping surveys have been applied, so that these represent our best estimates of a general relationship applicable to local star-forming galaxies. The gray band shows the observed 16%–84% range of R 21 for local galaxies from Leroy et al. (2022), and the slope of the inferred relations ﹩{R}_{21}\propto {I}_{\mathrm{MIR}}^{0.2}﹩ agrees well with recent results estimating the dependence of R 21 on ΣSFR.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: The 19 targets of the full PHANGS–JWST survey relative to our larger sample in I CO–I MIR space. As Figure 5, but each panel shows our compiled region-by-region data in gray with results, showing only CO (2–1). Red points show the subset of data for the 19 PHANGS–JWST targets. Though very slightly biased toward regions rich in CO emission, the full PHANGS–JWST survey reflects the larger galaxy population well and shows the same low-resolution CO (2–1) vs. mid-IR scalings that we observe in the rest of the local galaxy population.
Paper: PHANGS–JWST First Results: Destruction of the PAH Molecules in H II Regions Probed by JWST and MUSE
Authors: Oleg V. Egorov, Kathryn Kreckel, Karin M. Sandstrom, Adam K. Leroy, Simon C. O. Glover, Brent Groves, J. M. Diederik Kruijssen, Ashley. T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Eric Emsellem, Kathryn Grasha, Ralf S. Klessen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Erik Rosolowsky, Fabian Scheuermann, Eva Schinnerer, Jessica Sutter, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: JWST/MIRI images in the F770W, F1000W, and F1130W bands (red, green, and blue channels, respectively) of the four galaxies analyzed in this letter. Contours show the borders of individual H II regions selected from MUSE data, which meet the criteria in Section 3.1. Blue contours correspond to the H II regions with a hydrogen-ionizing photon rate Q 0 < 1050 s−1, and red contours correspond to those with Q 0 > 1050 s−1.
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption:  SCOUSEPY decomposition of the 30 pc resolution molecular CO(2−1) gas emission. Multiple Gaussian components are needed to fit ∼31% of the data. This is demonstrated most clearly in the spiral arms, where two- and three-component models are common (up to six components in the southwestern arm; top left). Spectra from selected regions with the resulting SCOUSEPY fits typically exhibit well-separated line components (top right). The inferred peak CO temperature and velocity dispersions of the individual SCOUSEPY components (bottom left) occupy a similar region of parameter space independent of whether they are derived from single or multiple-component fits (color-coding). The gray shaded regions correspond to the limits of our fitting (a signal-to-noise ratio of 2 and a single channel width). The three-dimensional representation of the individual SCOUSEPY components located within the white dashed box in the top left panel, displayed in ppv space (bottom right), reveals an inner smoothly rotating disk (highlighted in black; extracted from the ellipse in the top left panel), while the bar lanes show strong local fluctuations in velocity indicating an increasing complexity of the kinematics in the molecular gas there (the color refers to the peak CO temperature of the individual components). The physical spacing of the position–position grid in this image is ∼475 pc.
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption: Comparison of the distribution of the molecular gas and sites of ongoing star formation in the central ∼5 kpc of NGC 1365 in four different representations (north is up, and east is to the left). The ALMA CO(2−1) integrated intensity map (in color in the top left panel, in blue in the bottom right panel, and as blue contours in the remaining panels) basically traces the immediate gas reservoir for star formation. The JWST/MIRI 10 μm continuum map (in color in the bottom left panel and green in the bottom right panel) shows where the bright compact regions (cyan symbols, top panels) are likely tracing young (≤10 Myr) massive (≈106 M ⊙) star-forming regions. The PHANGS–MUSE Hα emission line map (Emsellem et al. 2022) at 1.″15 resolution (in color in the top right panel, in red in the bottom right panel, and as gray contours in the remaining panels) reveals the location of bright H II region complexes that are ionized by massive O stars. Regions of high attenuation (A  V  ≳  4 mag; Belfiore et al. 2022) are indicated by a yellow contour.
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption: Projected gas density and kinematic maps from a hydrodynamical simulation of a barred galaxy with NGC 1365–like properties. The selected snapshot broadly matches the properties of the gas in NGC 1365's inner disk. The central 5 × 3.5 kpc2 with the large-scale galactic bar position and disk orientation on sky matched to NGC 1365's properties. Top row: distribution of the gas mass (color) and stars formed in the past 10 Myr (green points) for the selected snapshot (middle). Comparison to two epochs showing the distributions 23 Myr earlier (left) and 6 Myr later (right) reveals the fast evolution of the morphology in just ∼30 Myr, which roughly corresponds to the dynamical time at a galactocentric radius of R gal = 1 kpc. Four prominent star clusters are labeled in the panels. The bottom row shows the properties of the molecular H2 gas: gas velocity field (left), H2 gas mass distribution (middle), and H2 gas velocity dispersion (right).
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption: In the left panel, refined molecular gas rotation curves using the 0.″3 CO velocity field are shown using the orientations from Lang et al. (2020; PA = 201°, inclination = 55°; black curve) and Gao et al. (2021; PA = 220°, inclination = 40°; orange curve). In the middle panel, the resulting residual velocity field when removing a circularly rotating disk (based on the inferred rotation curve using the Gao et al. 2021 orientation) clearly reveals strong streaming (i.e., noncircular) motions at the location of the gas lanes. In the right panel, the radial profile of the median molecular gas surface density (nominal curve: black solid line, assuming a 2 or 4× lower CO-to-H2 conversion factor: dashed and dotted lines, respectively) is compared to a number of stability criteria: virialized clouds (blue), Toomre critical density (red), and Roche density (orange). The gas in the inner disk (R gal ≤ 5″) is basically stable against gravitational collapse for all criteria considered (see text for details).
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption: Close-up look (5″ × 5″) at stellar populations in the inner disk (north is up, and east is to the left). The high sensitivity and resolution of the JWST/NIRCAM F200W imaging from PHANGS–JWST (left; Lee et al. 2023) reveals more structure in the region where undisturbed circular rotation gas has been found compared to what can be seen in the HST F814W map (right; Lee et al. 2022; Whitmore et al. 2023b, Whitmore et al. 2023a). Different regions that are discussed in the text are annotated. The bright (saturated) source to the east is the AGN at the center of NGC 1365.
Paper: PHANGS–JWST First Results: Rapid Evolution of Star Formation in the Central Molecular Gas Ring of NGC 1365
Authors: Eva Schinnerer, Eric Emsellem, Jonathan D. Henshaw, Daizhong Liu, Sharon E. Meidt, Miguel Querejeta, Florent Renaud, Mattia C. Sormani, Jiayi Sun, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Erik Rosolowsky, Karin M. Sandstrom, T. G. Williams, Ashley. T. Barnes, F. Bigiel, Mélanie Chevance, Yixian Cao, Rupali Chandar, Daniel A. Dale, Cosima Eibensteiner, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jaeyeon Kim, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Justus Neumann, Hsi-An Pan, Jérôme Pety, Toshiki Saito, Sophia K. Stuber, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore
Figure caption: Distribution of the emission from PAHs and hot dust emission as probed by JWST/MIRI observations at ∼0.″3 resolution, which is comparable to the resolution of the ALMA CO(2−1) data (north is up, and east is to the left). In the left panel, the F770W filter with an ∼0.″24 resolution reveals the overall distribution of the neutral ISM, as its emission is dominated by the 7.7 μm PAH feature. For reference, the distribution of the CO emission is shown by a single blue contour. Note that the central position is significantly affected by saturation due to the bright AGN and dominated by its PSF, causing the artifacts. Also, the three brightest compact sources north of the AGN are saturated. In the right panel, several embedded young star-forming clusters are evident in the 10 μm emission and stand out as bright compact sources. Our 10 μm–selected sources are highlighted by cyan diamonds and only found in the region shown. About 57% of these objects coincide with the young (<10 Myr) star clusters studied by Whitmore et al. (2023b; green crosses) and have estimated stellar masses of 106 M ⊙ or higher. The 21 μm–selected sources from Hassani et al. (2023) that are classified as ISM-emitting sources are shown as cyan circles. The dearth of clusters in the bar lane southwest of the nucleus is notable.