adsabs/AstroCLIMB huggingface dataset:
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: Molecular gas as probed by the CO(2−1) line emission from the inner 4.8 × 3.3 kpc2 of NGC 1365 at ∼30 pc (0.″3) resolution observed by ALMA. In the top panels, the integrated intensity distribution (left) reveals a faint smooth gas disk inside the prominent gas spiral arms. The white contour highlights I CO = 1000 K km s−1. The velocity field (right) shows circular rotation in the inner disk and clear deviations from this pattern at the locations of the gaseous bar lanes. The isovelocity contours are in steps of 40 km s−1 from the systemic velocity. In the bottom panels, the CO(2−1) peak temperature map (left) reveals several peaks reaching temperatures above 20 K, which often agree with peaks in the integrated intensity. Enhanced EWs (right) roughly coincide with the brightest emission in the bar lanes. The faint emission peak associated with the nucleus shows larger line widths above 40 km s−1.
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: Secondary dependence of the PAH fraction on the oxygen abundance of H II regions, measured as ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ (panel (a)); the F1130W/F770W flux ratio, sensitive to the relative fraction of neutral to ionized PAH (panel (b)); the number of hydrogen-ionizing photons Q 0 (panel (c)); and the equivalent width of Hα, corrected for the contribution of the underlying old stellar population (panel (d)). The 2D histograms in each panel show the distribution of ΔR PAH, obtained after subtracting the values derived by Equation (2) from the measured R PAH. The red dashed line shows a zero-difference level. The light blue dashed line in panel (a) corresponds to a linear fit defined by Equation (5), tracing the secondary relation of R PAH on metallicity. Spearman’s correlation coefficient (ρ) is given in the corner of each plot. Its uncertainty is derived in the same way as in Figure 2. The error bars in the right-hand corner correspond to the 95th percentile uncertainties of the measured values.
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 the PAH fraction, traced by R PAH, with different physical conditions. Panel (a): correlation with oxygen abundance, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩, with red symbols showing the mean value for each galaxy. Panel (b): equivalent width of Hα, EW(Hα), corrected for the contribution of the underlying old stellar population, and a tracer of H II region age. Note that because of the large uncertainty introduced by this background continuum subtraction, we consider here only regions with relative error δ(EW(Hα)) < 10%. Panel (c): log([O III]/Hβ), a tracer of the hardness of the UV radiation. Spearman’s correlation coefficient (ρ) is given in the corner of each plot. Its uncertainty is derived in the same way as in Figure 2. The error bars in the right-hand corner correspond to the 95th percentile uncertainties of the measured values.
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: Inner 5 kpc in the context of the large-scale stellar bar in NGC 1365. The optical color image from DES shows the 17 kpc long stellar bar (outlined by the orange ellipse as determined by Herrera-Endoqui et al. 2015) surrounded by spiral arms (left). In the zoom-in (marked as a gray box in the left panel), the bar lanes along the leading sides of the bar are highlighted via prominent extinction tracing dust (dark gray shaded) and the molecular gas distribution (blue shaded; top right). The field of view (FoV) under study in this work is shown as a dashed black box. The sketch (bottom right) outlines the basic structure of the orbits supporting the stellar bar (x 1: elongated along the bar major axis, in orange; x 2: elongated along the bar minor axis, in red) and the resulting bar lane morphology plus the inner star-forming ring. We further indicate the expected net gas flow and some relevant regions discussed in this work.
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: Dependence of [S III]/[S II] (left panel) and [O III]/Hβ (right panel) optical emission line ratios on the hardness of the ionizing UV radiation and the ionization parameter q, according to a grid of STARBURST99 and CLOUDY models (see text). Different points are the individual nodes of the model grid, defined by the different mass and age of the ionizing cluster and the density of the H II region. The color of the points encodes the number of hydrogen-ionizing photons, Q 0.
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: Same as Figures 2(a)–(c) but for the resolved H II regions only (those with R/PSF > 1 in Figure 2(d)). The colored lines show the same linear regressions as in Figure 2.
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: Same as Figure 6 but for a subsample of the H II regions with a large contrast against the surrounding local background in the Hα, [S II] emission lines, and mid-IR bands.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Left panel: mass ratio of NSC and host galaxy stellar mass (﹩{M}_{\star }^{\mathrm{nsc}}/{M}_{\star }^{\mathrm{gal}}﹩) vs. galaxy stellar mass. The NSC of NGC 628 is highlighted with a blue cross. Other data sets from the Local Volume (a field environment with a distance ≲11 Mpc; green diamonds; Seth et al. 2006; Georgiev et al. 2009a; Graham & Spitler 2009; Baldassare et al. 2014; Schödel et al. 2014; Calzetti et al. 2015; Carson et al. 2015; Crnojević et al. 2016; Nguyen et al. 2017; Baumgardt & Hilker 2018; Nguyen et al. 2018; Bellazzini et al. 2020; Pechetti et al. 2020), the Virgo galaxy cluster (orange squares; Sánchez-Janssen et al. 2019a), dwarfs around massive field galaxies (green triangles; Carlsten et al. 2022), and massive field galaxies (gray circles; GB14) show the general distribution of NSCs. The Milky Way NSC is highlighted with a blue plus sign. In comparison to other massive field late-type galaxies, the NSC of NGC 628 appears undermassive. Middle panel: effective radius (r eff) in the F814W vs. NSC stellar mass. The markers and colors of the data points are the same as in the left panel. Dashed lines give the mean density of clusters. Right panel: ellipticity (ϵ) vs. NSC stellar mass. We show the data by GB14 and color-code them by the host galaxy inclination. There is no apparent correlation between ellipticity, mass, and inclination. For NGC 628, the inclination has a value of i ∼ 8.°9 (Lang et al. 2020).
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Spectral flux density (S  ν ; left axis) and AB magnitude (m AB; right axis) vs. wavelength (λ). Different instruments are highlighted with marker symbols and colors. Red pentagons give the results by GB14 in the Vega magnitude system. Uncertainties are indicated with shaded areas. Two gray lines show the SED fits to the data including (dashed line) and excluding (solid line) the JWST MIRI data. The goodness of the fits is given by reduced χ 2 values in the panel. For both fits, we use the Bruzual & Charlot (2003) stellar population model and a delayed star formation history. The fit prefers a Chabrier (2003) initial mass function over the prescription by Salpeter (1955). Both fits indicate the presence of an 8 Gyr old stellar population with metallicity Z ∼ 0.02. No younger stellar population could be detected.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Main panel: central 5.″5 × 5.″5 of NGC 628 in JWST MIRI F2100W. A darker shade and white contours show high flux in F2100W. Red contours highlight the HST WFC3 F275W emission. Both maps are matched based on the most up-to-date world coordinate solutions. Inset panel: zoom into the nucleus of NGC 628. The white and red contours again highlight the emission in F2100W and F275W, respectively. The offset between the centers of the contours measures approximately 0.″2.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Angular separation (θ) vs. wavelength (λ) of the NSC position with respect to HST WFC3 F275W. Different instruments are highlighted with different symbols and colors. Crosses show the angular separation of a star with Gaia EDR3 designation 2589386446469602688. The vertical length of the cross gives 0.5 pixel, which we assume as an upper limit on extracting the position of the star. Data points above the crosses indicate that either the WCS is offset or the center of the nucleus is offset compared to HST WFC3 F275W. In some bands (for example, HST ACS F814W), the star is saturated, and no central position could be determined. The separations for a GC located ∼10″ southwest of the nucleus are shown with black hexagons. The offsets agree with the offsets of the star in the NIRCam data.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Structural properties of the nucleus of NGC 628: effective radius (panel (a)), ellipticity (panel (b)), Sérsic index (panel (c)), and position angle (panel (d)) vs. wavelength. Marker symbols and colors highlight different instruments. Uncertainties are shown with shaded areas. Red pentagons show literature values from GB14.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Overview of the same central region as in Figure 3 but for available JWST NIRCam and MIRI data. For F2100W, no fit was possible, including PSF convolution. The model shown here is a pure Sérsic profile without PSF convolution to determine the apparent magnitude of the source. For the MIRI data, we adjust the gray scales to 0.99 and 1.01 times the mean.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Overview of the central 5.″5 × 5.″5 (1″ ≈ 47 pc) of NGC 628 in six different HST bands. North is up, and east is left. Top row: data products as used for fitting. Middle row: model images of the best fit using one Sérsic profile for the NSC, an additional Sérsic profile for the background, and a plane offset. Bottom row: residual map, data − model. The gray scales of the maps are logarithmic and vary from 5 × 10−3 to 5 × 10−2 times the mean of the residuals.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Logarithmic fraction of the number of AGB stars multiplied by their mass and divided by the total NSC mass (﹩{\mathrm{log}}_{10}\,f﹩) vs. AGB star mass. Each data point is color-coded according to the age of the star. Note that all AGB stars are younger than the main stellar population of the NSC, as identified by fitting the SED.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Transmission of the HST and JWST bands used in this work.
Paper: PHANGS–JWST First Results: A Combined HST and JWST Analysis of the Nuclear Star Cluster in NGC 628
Authors: Nils Hoyer, Francesca Pinna, Albrecht W. H. Kamlah, Francisco Nogueras-Lara, Anja Feldmeier-Krause, Nadine Neumayer, Mattia C. Sormani, Médéric Boquien, Eric Emsellem, Anil C. Seth, Ralf S. Klessen, Thomas G. Williams, Eva Schinnerer, Ashley. T. Barnes, Adam K. Leroy, Silvia Bonoli, J. M. Diederik Kruijssen, Justus Neumann, Patricia Sánchez-Blázquez, Daniel A. Dale, Elizabeth J. Watkins, David A. Thilker, Erik Rosolowsky, Frank Bigiel, Kathryn Grasha, Oleg V. Egorov, Daizhong Liu, Karin M. Sandstrom, Kirsten L. Larson, Guillermo A. Blanc, Hamid Hassani
Figure caption: Overview of the nuclear region of NGC 628 in different bands. Each panel gives the central 20″ × 20″ (approximately 950 pc × 950 pc) of the galaxy, centered on the NSC. North is up, and east is to the left. Color correlates with intensity. The first row gives three color images using the HST and JWST bands highlighting star formation by using the continuum-subtracted HST ACS F658N (Hα) filter. Dust lanes, where star formation occurs, are clearly visible in the first and third panels, while only stellar emission is shown in the second panel. The square box of side length 5.″5 in the third panel shows the region we considered for the fit of the NSC. The second row highlights other available data sets, namely, the AstroSat UV emission, MUSE Hα, and ALMA CO. The first two panels again trace star formation, whereas the third panel shows the location of the molecular gas. Note the absence of star formation and gas in the immediate vicinity of the NSC, which is marked with a white cross. The third and fourth rows show the HST data increasing in wavelength. Star-forming regions identified in the HST WFC3 F275W become hidden behind dust filaments in other bands. The sixth panel (in the fourth row), showing the HST ACS F814W data, mainly shows stellar emission. We show the newly obtained JWST NIRCam (fifth) and MIRI (sixth) in the last two rows, again in increasing wavelength from near- to mid-infrared. The NIRCam data highlight the stellar emission, while the MIRI data show both stellar and dust emission. As for the molecular gas (ALMA CO; second row), a central cavity exists, and dust is present in the spiral arms of NGC 628.