adsabs/AstroCLIMB huggingface dataset:
Paper: Observational Evidence for Cosmological Coupling of Black Holes and its Implications for an Astrophysical Source of Dark Energy
Authors: Duncan Farrah, Kevin S. Croker, Michael Zevin, Gregory Tarlé, Valerio Faraoni, Sara Petty, Jose Afonso, Nicolas Fernandez, Kurtis A. Nishimura, Chris Pearson, Lingyu Wang, David L Clements, Andreas Efstathiou, Evanthia Hatziminaoglou, Mark Lacy, Conor McPartland, Lura K Pitchford, Nobuyuki Sakai, Joel Weiner
Figure caption: (Vertical bars) Fraction of z = 0 halo density contributed by k = 3 BHs, as produced by the indicated SFRDs in Figure 2. Models are ordered by increasing SFRD power-law slope, with colors set to agree with the model lines in Figure 2. Also displayed (gray, shaded) are current constraints on MACHOs from microlensing (Blaineau et al. 2022), wide halo binary disruption (Monroy-Rodríguez & Allen 2014; Tyler et al. 2022), and ultra-faint dwarf (UFD) galaxy disruption (Brandt 2016). Noting the broken vertical axis, the microlensing and halo binary constraints are easily satisfied. Dwarf galaxy constraints may discriminate candidate SFRD and IMF combinations. As shown, UFD constraints are overly conservative because they do not account for the decrease in comoving BH mass density at earlier times, as will be present in the k > 0 coupled scenario. The effects of accretion at z > 7, as well as adopting a top-heavy IMF (Appendix A), are visible as a decreased fraction in the intermediate-mass BH range. Horizontal bars show the fraction of present-day ΩΛ contributed by each mass bin. Mass bins that contribute <5% of ΩΛ are unlabeled for clarity. Color gradients indicate mass binning and are common to both vertical and horizontal bars. Contributions less than 1%, including negligible contributions omitted in the vertical bars, are also shown in log scaling. Here, contributions are ordered by density fraction.
Paper: Observational Evidence for Cosmological Coupling of Black Holes and its Implications for an Astrophysical Source of Dark Energy
Authors: Duncan Farrah, Kevin S. Croker, Michael Zevin, Gregory Tarlé, Valerio Faraoni, Sara Petty, Jose Afonso, Nicolas Fernandez, Kurtis A. Nishimura, Chris Pearson, Lingyu Wang, David L Clements, Andreas Efstathiou, Evanthia Hatziminaoglou, Mark Lacy, Conor McPartland, Lura K Pitchford, Nobuyuki Sakai, Joel Weiner
Figure caption: (Top) Posterior distributions of cosmological coupling strength k, inferred by comparing supermassive black holes (BHs) in local elliptical galaxies to those in five samples of elliptical galaxies at z > 0.7. (Bottom) Combining these posterior samples with equal weighting gives a distribution with ﹩k={3.11}_{-1.33}^{+1.19}﹩ at 90% confidence. If fit to a Gaussian, the fit has a mean of k = 3.09 with a standard deviation of 0.76 (shading). Vertical lines indicate: k = 0 coupling, as expected for traditional BHs like Kerr and the decoupled solution by Nolan (1993); and k = 3 coupling, as predicted for vacuum energy interior BHs. The measurement disfavors zero coupling at 99.98% confidence and is consistent with BHs possessing vacuum energy interiors, as first suggested by Gliner (1966).
Paper: PHANGS–JWST First Results: Interstellar Medium Structure on the Turbulent Jeans Scale in Four Disk Galaxies Observed by JWST and the Atacama Large Millimeter/submillimeter Array
Authors: Sharon E. Meidt, Erik Rosolowsky, Jiayi Sun, Eric W. Koch, Ralf S. Klessen, Adam K. Leroy, Eva Schinnerer, Ashley. T. Barnes, Simon C. O. Glover, Janice C. Lee, Arjen van der Wel, Elizabeth J. Watkins, Thomas G. Williams, F. Bigiel, Médéric Boquien, Guillermo A. Blanc, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin M. Sandstrom, Rowan J. Smith, Mattia C. Sormani, David A. Thilker
Figure caption: Comparison between the spacings measured for filaments detected by FilFinder (black) and estimates for the Jeans length, Toomre length, most unstable 2D wavelength, and gas scale height (gray, blue, red, and purple hatched regions) in (clockwise from top left) NGC 628, IC 5332, NGC 7496, and NGC 1365. In NGC 628 and IC 5332 the average azimuthal filament spacings in 300 pc wide (projected) radial bins are shown. In NGC 1365 and NGC 7496, the average radial filaments spacings in two radial zones, R < 2.5 kpc and R > 2.5 kpc, are shown. The dark gray bar depicts the Jeans length estimated (where possible) using a determination of the equilibrium gas scale height shown in red (see Section 3.2), while the light gray band shows the range of values implied adopting a fixed 100 pc scale height. The light blue band traces the range in Toomre lengths estimated for each gas disk. The purple band shows the value estimated for λ 2D where 2D structure preferentially forms as long as Q does not exceed unity. Note that, given the estimated λ  T , these λ 2D estimates would all coincide with Q > 1, disfavoring structure on this scale (see Equation [1]). Additional hatched light gray and light blue bands for IC 5332 show, respectively, the Jeans length (forward hatch) and Toomre length (backward hatch) when an atomic gas component is included, assuming a constant h = 100 pc.
Paper: PHANGS–JWST First Results: Interstellar Medium Structure on the Turbulent Jeans Scale in Four Disk Galaxies Observed by JWST and the Atacama Large Millimeter/submillimeter Array
Authors: Sharon E. Meidt, Erik Rosolowsky, Jiayi Sun, Eric W. Koch, Ralf S. Klessen, Adam K. Leroy, Eva Schinnerer, Ashley. T. Barnes, Simon C. O. Glover, Janice C. Lee, Arjen van der Wel, Elizabeth J. Watkins, Thomas G. Williams, F. Bigiel, Médéric Boquien, Guillermo A. Blanc, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin M. Sandstrom, Rowan J. Smith, Mattia C. Sormani, David A. Thilker
Figure caption: JWST/MIRI 11.3 μm images (top) and FilFinder masks (bottom; see Section 3.1.1) for two PHANGS–JWST targets, NGC 0628 (left) and IC 5332 (right). The MIRI images are displayed on a asinh stretch. The physical scale is indicated by a white bar in the top panels, while the red ellipses in the bottom panels positioned at a galactocentric radius R = 2 kpc mark the orientation of elliptical annuli in the azimuthal spacings of the filaments identified in these two galaxies.
Paper: PHANGS–JWST First Results: Interstellar Medium Structure on the Turbulent Jeans Scale in Four Disk Galaxies Observed by JWST and the Atacama Large Millimeter/submillimeter Array
Authors: Sharon E. Meidt, Erik Rosolowsky, Jiayi Sun, Eric W. Koch, Ralf S. Klessen, Adam K. Leroy, Eva Schinnerer, Ashley. T. Barnes, Simon C. O. Glover, Janice C. Lee, Arjen van der Wel, Elizabeth J. Watkins, Thomas G. Williams, F. Bigiel, Médéric Boquien, Guillermo A. Blanc, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin M. Sandstrom, Rowan J. Smith, Mattia C. Sormani, David A. Thilker
Figure caption: JWST/MIRI 11.3 μm images (top) and FilFinder masks (bottom; see Section 3.1.1) for two PHANGS–JWST targets, NGC 1365 (left) and NGC 7496 (right). The MIRI images are displayed on a asinh stretch. The physical scale is indicated by a white bar in the top panels, while the red lines in the bottom panels illustrate the orientation of one of the segments along which radial spacings are measured in these two galaxies (deprojected).
Paper: PHANGS–JWST First Results: Interstellar Medium Structure on the Turbulent Jeans Scale in Four Disk Galaxies Observed by JWST and the Atacama Large Millimeter/submillimeter Array
Authors: Sharon E. Meidt, Erik Rosolowsky, Jiayi Sun, Eric W. Koch, Ralf S. Klessen, Adam K. Leroy, Eva Schinnerer, Ashley. T. Barnes, Simon C. O. Glover, Janice C. Lee, Arjen van der Wel, Elizabeth J. Watkins, Thomas G. Williams, F. Bigiel, Médéric Boquien, Guillermo A. Blanc, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, J. M. Diederik Kruijssen, Kirsten L. Larson, Daizhong Liu, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Toshiki Saito, Karin M. Sandstrom, Rowan J. Smith, Mattia C. Sormani, David A. Thilker
Figure caption: Kernel density estimate of histograms of Toomre Q values for the gas in the four target galaxies calculated from observed gas properties across each CO-emitting disk. The dashed (solid) red line for IC 5332 shows the Q values estimated with (without) an atomic gas component.
Paper: Hydrodynamical Simulations of Black Hole Binary Formation in AGN Disks
Authors: Jiaru Li, Adam M. Dempsey, Hui Li, Dong Lai, Shengtai Li
Figure caption: Evolution of r 1 (blue) and r 2 (orange) around the time when the BHs encounter each other for our main suite of simulations. The simulations are grouped by disk mass (rows; increasing from bottom to top, with ﹩{{\rm{\Sigma }}}_{0}{R}_{0}^{2}/M={10}^{-5}﹩, 5 × 10−5, and 10−4) and initial azimuthal separation of the two BHs Δφ (columns; increasing from left to right, with Δφ = 30°, 60°, 90°, 120°, 150°, and 180°). Generally, we find that the likelihood of binary capture increases as the disk mass increases. But large initial azimuthal separations can hinder formation.
Paper: Hydrodynamical Simulations of Black Hole Binary Formation in AGN Disks
Authors: Jiaru Li, Adam M. Dempsey, Hui Li, Dong Lai, Shengtai Li
Figure caption: Orbital evolution of all bound binaries in our main suite of simulations. From top to bottom we plot the time evolution of the BH separation, binding energy in units of E Hill = −Gm  b /(2R H) (or equivalently the ratio of R H to the binary semimajor axis a b), eccentricity, and specific angular momentum. Binaries form via multiple close encounters that collectively dissipate a large amount of the BHs’ kinetic energy. Once formed, all binaries are retrograde and eccentric. Over time, their eccentricities dampen and they tighten to our resolution limit.
Paper: Hydrodynamical Simulations of Black Hole Binary Formation in AGN Disks
Authors: Jiaru Li, Adam M. Dempsey, Hui Li, Dong Lai, Shengtai Li
Figure caption: Snapshots of the gas surface density and power per unit area delivered to the BHs for the exemplary simulation dp30high at three different times before and after the first close encounter. At early times (left column), each BH supports a CSD and trailing Lindblad spirals. Just before close encounter, the CSDs collide (middle column). As the BHs depart (right column), the CSD gas is left behind and drags the BHs (﹩{\dot{\varepsilon }}_{\mathrm{gas}}\lt 0﹩), slowing them down.
Paper: Hydrodynamical Simulations of Black Hole Binary Formation in AGN Disks
Authors: Jiaru Li, Adam M. Dempsey, Hui Li, Dong Lai, Shengtai Li
Figure caption: Time evolution of the binding energy for the simulation shown in Figure 3 (top panel) as well as radial profiles of the gas linear mass density (bottom left) and cumulative power delivered to the binary (bottom right) at five different times (shown on the top panel). Times 1–5 correspond to T = 534.210 P 0, 534.213 P 0, 534.214 P 0, 534.215 P 0, and 534.218 P 0, respectively. The Σ and ﹩\dot{\varepsilon }﹩ maps for times 2 and 4 are shown in Figure 3. Before the first close encounter (curves with left-pointing arrows), most of the gas tracks the BHs. After the close encounter (curves with right-pointing arrows), most of the mass remains near the interaction site (δ r ∼ 0) and removes a significant amount of energy from the BHs. This is in agreement with the 2D picture shown in Figure 3.
Paper: Hydrodynamical Simulations of Black Hole Binary Formation in AGN Disks
Authors: Jiaru Li, Adam M. Dempsey, Hui Li, Dong Lai, Shengtai Li
Figure caption: Scatterplot of close encounter outcomes for our expanded set of simulations. The y-axis encodes the mass scale of the AGN disk, while the x-axis shows the value of E b just before the first close encounter (evaluated when r b = 0.3 R H) in units of ∣E Hill∣ = Gm b/(2R H). We color each point by whether or not the BHs catch into a bound system. In this space there is a clear dividing line between formation and no-formation that we mark with a gray line and provide a numerical fit for in Equation (7).
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: (a) Rest-frame UV spectrum of A2744-arc3 extracted from the VLT/MUSE 3D data cube, with the error spectrum shown in red. Nebular emission lines and absorption features associated with A2744-arc3 are labeled with dashed red and blue lines, respectively A series of absorption features from an intervening Fe II absorber at z = 2.582 are identified in orange. (b) Normalized spectrum zoomed into the DLA Lyα and Lyβ line profiles with the Voigt profile fits, with flux uncertainties indicated by gray shaded region. The red solid lines imply the best-fit result yielding ﹩\mathrm{log}({N}_{{\rm{H}}\,{\rm\small{I}}}/{\mathrm{cm}}^{-2})=21.8\,\pm \,0.1﹩. Tentative residual in the trough is identified by the red shaded region. (c) Normalized spectrum zoomed into the metal absorption-line profiles. The blue shaded regions are used to measure the equivalent width (EW) of the absorbers. A tentative velocity offset of −36 km s−1 relative to z = 3.980 (blue dashed) is marked in green dashed lines. (d) The neutral gas metallicity derived from the O I absorber in compared with metal abundances of DLAs (Rafelski et al. 2012; gray squares) and Lyman break galaxies (LBGs; Troncoso et al. 2014; blue triangles) out to z = 5. The gray dashed lines indicate the cosmic evolution of DLA metallicities in Rafelski et al. (2012). The gray shaded region marks metallicities lower than solar values. The purple star marks the H II region [O/H] abundance of A2744-arc3 derived from [Ne III]/[O II] empirical metallicity calibrations, as described in Section 4.2.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: The UV slope β map in the image plane and source plane measured from HST and JWST broadband images. The HST UV slope maps are measured from WFC3/F105W, F125W, F140W, and F160W images (2125–3091 Å in the rest frame), while the JWST UV slope maps are constructed only using NIRISS/F115W and F150W images (2315–3015 Å in the rest frame), to avoid emission lines captured by the NIRISS/F200W filter. The overlaid green contours in HST image/source plane denote the lensed/delensed WFC3/F160W surface brightness levels of 0.05, 0.075, 0.1 MJy sr−1, and the contours in JWST image/source plane show NIRISS/F150W lensed/delensed surface brightness levels of 0.075, 0.1, 0.135 MJy sr−1 respectively. The ellipses on the upper right corners correspond to the FWHM of image/source-plane point-spread function (PSF). Note that source-plane PSF varies among positions due to different magnification and distortion, and the shown one is with the largest FWHM determined by deflection fields at one of the three clumps.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: The schematic toy model of A2744-arc3 as a low-mass, low-metallicity galaxy with high-metallicity neutral gas reservoir. The blue stellar clumps inside mark the compact and bursty star-forming regions in A2744-arc3, on scales of subkiloparsecs. Their hard ionization field forms hot, thin, and highly ionized H II regions around them, where strong narrow nebular emission lines are produced. The gas outer layer denotes the neutral gas reservoir with varying column densities in the CGM. Its geometry determines the shape of Lyα emission/absorption we observed. When sightlines are blocked by high-column-density gas, damped Lyα absorption is observed; in partially obscured case, Lyα emission with underlying absorption is observed. Three arrows mark possible gas cycles within the galaxy. Feedback from central star formation, such as stellar winds, could metal enrich the neutral gas, leading to strong metal absorbers with P-Cygni profiles. The recycled neutral gas can further efficiently fuel the next-generation star formation.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: Top left: JWST NIRISS F150W surface brightness image of A2744-arc3 with overlaid continuum contours of ALMA band 6. The contours levels are −2 (white dashed), 1 and 2σ (white solid) with 1σ = 44.5 μJy beam−1, showing no clear detection at a rest-frame wavelength of 0.23 mm. Top right: photometry and SED fitting for A2744-arc3, with derived physical parameters. Blue triangles denote the measurement and red circles the best-fit result. Bottom: optimally extracted 1D spectra (top panel) and joint 2D spectra covered by NIRISS three filters (F115W, F150W, and F200W). In the top panel, shaded blue regions indicate flux uncertainties, and vertical red lines label common emission lines, among which Mg II is not detected. The 2D spectra of the bottom panel are obtained by summing 2D spectra of the five segments as described in Section 2.1.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: Reconstructed UV slope distribution on the source plane using JWST/NIRISS images. The left panel shows the reconstruction for the east side of A2744-arc3 using the Glafic model. The middle presents the reconstruction for the west side of A2744-arc3 with the R21 model and the right for its east part. See more details in Figure 2.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: Photometry and SED analysis of A2744-arc3, with delensed fluxes measured using Richard et al. (2021) lensing model. The blue triangles denote the measurement and the red circles the best-fit result. Although the adopted lensing model is different, these R21 results are very consistent with that shown in Figure 1.
Paper: Metal-enriched Neutral Gas Reservoir around a Strongly Lensed Low-mass Galaxy at z = 4 Identified by JWST/NIRISS and VLT/MUSE
Authors: Xiaojing Lin, Zheng Cai, Siwei Zou, Zihao Li, Zuyi Chen, Fuyan Bian, Fengwu Sun, Yiping Shu, Yunjing Wu, Mingyu Li, Jianan Li, Xiaohui Fan, J. Xavier Prochaska, Daniel Schaerer, Stephane Charlot, Daniel Espada, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Stark, Kirsten K. Knudsen, Gustavo Bruzual, Jacopo Chevallard
Figure caption: Voigt profile fits to the Al II λ1670, Fe II λ1608, O I λ1302, Si II λ1526, and Si IV λ1402 absorbers, assuming two components for each absorbers and fixing the Doppler parameters b to 5, 10, 15, and 30 km s−1. Red lines are the best-fit profiles and the blue vertical lines mark the positions of the two components for each absorber. The top row of each panel shows residuals of the best-fit profiles (black) and 3σ uncertainties (red dashed). The total column density of each absorber, obtained by summing over their two components, is labeled, in units of logN cm−2.
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: Multi-scale bubble population in NGC 628 revealed with JWST observations. RGB illustration toward the center of NGC 628 highlighting bubble features and the bands used in their identification. Red traces MIRI F770W observations, green traces MUSE Hα observations, and blue traces B-band HST observations. White scalebar indicates physical size equal to 1 kpc.