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Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Bubble locations identified in NGC 628 with multi-scale view zoom ins providing a more detailed view. Left: MIRI F770W band map of NGC 628 using a square root intensity stretch. Cyan ellipses show the location of the 1694 bubbles identified. Labeled lines indicate position of spiral arms derived by skeletonizing the arm environment masks from Querejeta et al. (2021). Solid circle markers on arm spines indicate the start position of the arm. White boxes labeled a and b indicate locations of close-up panels on right side of this figure. Right: same RGB as Figure 1 but focused on the regions indicated on the left panel. Bars at bottom left indicate the physical size scale.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Size distributions of bubbles. Top: size distribution of the entire sample of bubbles. Solid gray and red lines are the mean and median of the distribution, respectively, shaded blue region is the 16th–84th sigma range (labeled as σ in the legend), and dashed cyan line is the power-law fit to the distribution equal to p = − 2.2 derived using MLE. Inset shows the bootstrapped distribution of the power-law index in the bottom panel with a central value of −2.2 with a 16th–84th sigma range of −2.3–2.1. Middle: total number of nested bubbles within the boundary of a larger bubble. The x-axis corresponds to the radius of the larger bubble. White distribution shows the data while coral shows the same distribution if instead bubble locations were randomized, averaged over 100 different randomized realizations. Bottom: size distribution for bubbles upstream and downstream from a spiral arm, shown in orange and blue, respectively, with the same colored lines showing their 99th percentile values. A Mann–Whitney test comparing the two distributions indicates 0.01% chance that the two distributions are equal.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Offset angles between elliptical bubbles and the spiral-arm tangent angle. Top: solid black and blue lines with apertures show offset angles for bubbles with aspect ratios >1 and >1.15, respectively, for bubbles with an uncertainty in measured angle of ±5°, resulting in a KDE-like distribution. The blue line has been renormalized to match the area of the black line (i.e., from 301 bubbles to 654 bubbles) to make comparisons easier. Translucent regions indicate the uncertainty. Dashed red line shows the distribution of offset angles if bubbles have random PAs. Bottom: same as blue line in top panel (i.e., AR > 1.15) but for bubbles >40 pc upstream (black) and downstream (purple) from an arm.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Multiwavelength observations covering the nearby star-forming galaxy NGC 628. In the top row of panels from left to right, we show the Hα map from PHANGS-MUSE (Emsellem et al. 2022), CO(2–1) peak intensity from PHANGS-ALMA, (Leroy et al. 2021), and the Very Large Array (VLA) HI moment 0 map from the THINGS survey (Walter et al. 2008). In the middle row, left panel, we show an image produced from the B- (blue), V- (green) and I- (red) band filters from HST, and the continuum-subtracted HST Hα (658 nm, red; see Lee et al. 2022). In the middle center and right panels, we show the UV emission map from AstroSat (H. Hassani et al. 2022, in preparation) and NIRCam F335M emission from JWST (Lee et al. 2023). On the bottom row, from left to right, we show the 8 μm map from Spitzer (Dale et al. 2009), and the F770W and the F2100W maps from MIRI JWST (Lee et al. 2023). All panels have been overlaid with a dashed contour showing the coverage of the JWST observations.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Close-up view of bubble features in NGC 628. From left to right, we show complex, nested bubbles where we might have mischaracterized the bubbles present; bubbles downstream from an arm with sheared features upstream; and a closer look at the sheared features shown on the previous panel. These RGB images have the same bands and scaling as in Figures 1 and 3.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: KDE distributions of bubble sizes binned as a function of galactocentric distance in 1 kpc rings. Dashed and solid black lines show the median and mean values, while the solid pink, red, and cyan lines show the 84th, 95th, and the 99th percentiles, respectively. The color of the distributions shows the number of bubbles per unit surface area in annular rings at the distance indicated on the y-axis. The number labeling each distribution indicates the number of bubbles within the distribution.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Bubble age as a function of galactocentric distance. The dashed blue and solid orange lines are the bubble ages for mean and median bubble ellipticity, respectively.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Left: same as Figure 3 for catalog B. Right: same as Figure 3 for catalog C.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Close-up view of a bubble potentially missing from the catalog. Translucent black ellipse highlights a large (>500 pc) feature that could be a missing large bubble that is too sheared to confirm unambiguously. RGB image with the same bands and scaling as in Figures 1 and 3.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Left: same as Figure 3 for catalog B but with the bottom panel removed. Right: same as Figure 3 for catalog C but again with the bottom panel removed.
Paper: PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628
Authors: Elizabeth J. Watkins, Ashley T. Barnes, Kiana Henny, Hwihyun Kim, Kathryn Kreckel, Sharon E. Meidt, Ralf S. Klessen, Simon C. O. Glover, Thomas G. Williams, Benjamin W. Keller, Adam K. Leroy, Erik Rosolowsky, Janice C. Lee, Gagandeep S. Anand, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Rupali Chandar, Ness Mayker Chen, Mélanie Chevance, Enrico Congiu, Daniel A. Dale, Sinan Deger, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Cinthya Herrera, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Laura A. Lopez, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin Sandstrom, Fabian Scheuermann, Eva Schinnerer, Mattia C. Sormani, Sophia K. Stuber, David A. Thilker, Antonio Usero, Bradley C. Whitmore
Figure caption: Left: same as Figure 3 for catalog B. Right: same as Figure 3 for catalog C. We note here that the color of the distribution between 0 and 1 kpc is 31 kpc−2 for catalog C.
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Comparison of a feedback-driven bubble and its host stellar population for the Phantom Void and the Precursor Phantom Void (also shown in Figure 1). From left to right in upper panels, we show the JWST 7.7 μm, HST Hα, and the NUV (F275W) filters. Overlaid as colored contours on the upper-right panel is the age of the stellar associations (at a scale of 32 pc; see Deger et al. 2020). From left to right in the center panels are the Spitzer 8 μm (Dale et al. 2009), MUSE Hα (Emsellem et al. 2022), and Astrosat NUV (Hassani et al. 2023) observations. In the bottom panels are the ALMA CO (Leroy et al. 2021a), VLA H I (Walter et al. 2008), and HST broadband (Lee et al. 2022) observations. The white dashed line in all panels denotes the bubble and shell of each region (see Figure 7). We find that young and high-mass stellar associations (<20 Myr; >105 M ⊙) exist within the bubble (particularly toward the boundaries), highlighting these as good candidates for driving the bubble expansion.
Paper: PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hamid Hassani, Erik Rosolowsky, Adam K. Leroy, Médéric Boquien, Janice C. Lee, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Sharon E. Meidt, Karin M. Sandstrom, Eva Schinnerer, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Correlation between luminosity in the extinction-corrected Hα line as a function of 21 μm luminosity density. The color bar shows the age of the sources, and the total stellar mass of each region is represented by its size. Both age and mass are estimated via SED fitting using CIGALE (Section 5.1). Most regions show an excellent correlation between 21 μm and Hα luminosity. The black dashed line indicates the threshold below which we regard a 21 μm source as being Hα-faint (L Hα /ν L  ν,F2100W = 0.05 < 1/80), and the red line indicates the mean L Hα /ν L  ν,F2100W = 0.05. The vertical line at L  ν  = 1019 W Hz−1 is the threshold below which we search for embedded sources. We plot representative fractional error bars in the bottom of the plot in five different L  ν,F2100W ranges.
Paper: PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hamid Hassani, Erik Rosolowsky, Adam K. Leroy, Médéric Boquien, Janice C. Lee, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Sharon E. Meidt, Karin M. Sandstrom, Eva Schinnerer, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Luminosity distribution of 21 μm sources classified as ISM sources in the JWST MIRI data. The distributions are grouped by host galaxy in order of increasing distance (top to bottom). The blue dotted lines indicate the mean 5σ error in source luminosity. The red lines indicate a fit to the power-law distribution with ﹩{dN}/{{dL}}_{\nu }\propto {L}_{\nu }^{\beta }﹩ over 2 orders of magnitude. The value of β is labeled in each panel. The mass scale on the top axis translates the luminosity measurements to equivalent masses using the median ratio we determine from SED fitting (Section 5.1).
Paper: PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hamid Hassani, Erik Rosolowsky, Adam K. Leroy, Médéric Boquien, Janice C. Lee, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Sharon E. Meidt, Karin M. Sandstrom, Eva Schinnerer, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Color–color plots of the 21 μm–selected sources in the MIRI (left) and NIRCam (right) bands constructed from band ratios that highlight significant PAH emission for z = 0 sources. Dashed lines indicate loci that partition the color–color space into sources with bright ISM emission (ISM) vs. background galaxies (HZ) and extreme-AGB stars that lack a PAH feature (STAR). Classifications are made by eye in examining the full SED and morphology of sources in the full PHANGS data set. The L20 line indicates the proposed line for stellar colors from Lai et al. (2020). The green line in the right panel indicates the expected flux ratios for PAH emission in Sandstrom et al. (2023b).
Paper: PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hamid Hassani, Erik Rosolowsky, Adam K. Leroy, Médéric Boquien, Janice C. Lee, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Sharon E. Meidt, Karin M. Sandstrom, Eva Schinnerer, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: The RGB maps of NGC 7496 (top left), NGC 0628 (top right), NGC 1365 (bottom left), and IC 5332 (bottom right) at wavelengths of 21 (red), 10 (green) and 7.7 + 11.3 (blue) μm. The red zoom-in windows show peaks at 21 μm (black circles), background galaxies (red diamonds), H II regions (blue squares), MSAs (gray stars), and compact stellar clusters (orange stars). In total, 1271 sources are found throughout the images, but we only show symbols in the inset images to reduce crowding. We also highlight some representative background galaxies in the blue zoom-in windows, showing the F200W data at their native resolution.