adsabs/AstroCLIMB huggingface dataset:
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Mass fraction of the largest remnant as a function of ﹩{Q}_{\rm{R}\,}/{Q}_{\,\rm{RD}}^{\star }﹩, for orbital distance δ considering only radial (-R) collisions with Mproj/Mtarg = 0.1. A unique ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ is determined for each fixed δ. For each set of dots corresponding to a fixed δ, a unique ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ is determined by performing a linear fit to the universal disruption law (Equation (2)). The simulations match the “universal law” quite well for δ ≳ 3
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Concentric annuli used to extract the radial brightness profiles of the radio halos in PLCK G287.0+32.9 (50″  resolution), A2744 (25″  resolution), Bullet (15″  resolution), MACS J0717.5+3745 (20″  resolution), and A2142 (75″  resolution; image adopted from L. Bruno et al. 2023). The hatched areas indicate the masked regions. The width of each circular annulus is half the FWHM of the beam size. The last panel illustrates the different azimuthal annuli (elliptical and partial elliptical) used to investigate the radial profiles of the PLCK G287+32.9 halo, with the resulting profiles shown in Figure 12 top-right panel. The last panel image of PLCK G287.0+32.9 is obtained by subtracting discrete sources using an inner uv-cut. For the rest of the image properties, see Table 4 (IM7, IM12, IM15, and IM19). We emphasize that the masked regions differ between the PLCK G287.0+32.9 maps with masking and those with uv-subtraction (see first and last panel images).
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Radial radio profiles of the halos in PLCK  G287.0+32.9, A2744, Bullet, and MACS J0717+3745 at difference frequencies. The kinks in the radial profiles of the Bullet Cluster halo and A2744 (gray shaded regions) are due to shock fronts. To avoid overlap, the surface brightness profiles for PLCK G287.0+32.9 at 2.4 GHz, 815 MHz, and 350 MHz have been scaled by factors of 0.76, 1.5, and 2.5, respectively. Similarly, the A2744 profile at 815 MHz is scaled by a factor of 2. The surface brightness is measured in circular annuli (see Figure 7 for the chosen annuli), and the data are fitted with single-component exponential profiles. The PLCK  G287.0+32.9, A2744, Bullet Cluster, and MACS J0717+3745 profiles are extracted from 50″, 25″, 15″, and 20″  resolution maps, respectively. The width of the annuli is half of the beam FWHM. At all the observed frequencies, the halo emission can be described by a single component.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Radial profiles of the halos in A2142 (left) and PLCK G287.0+32.9 (right). Profiles fitted with a single-component exponential model are shown with dashed lines. The used annuli are shown in Figure 7 Left: Radial profile of the A2142 halo at 144 MHz, extracted from an image where unrelated sources were masked based on the LOFAR HBA map (red data points) and from an image where unrelated sources were masked using the sensitive 1.3 GHz MeerKAT map (light coral data points). The blue data points/line show the residual radial profile obtained subtracting the uv-subtracted sources profile from the masked-out sources profile. Top right: PLCK G287.0+32.9 halo profiles at 815 MHz and 350 MHz obtained after subtracting discrete sources from the uv-data. Both plots exhibit a second outer component resulting from the incomplete subtraction of discrete sources.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: MAC J0717 LOFAR HBA (120–167 MHz) and A2142 (120–167 MHz) full band continuum radio images in square-root scale. The central region of MAC J0717 is dominated by a bright relic, projected on the halo emission (K. Rajpurohit et al. 2021a). The halo in A2142 is extended along the northwest to southeast direction (L. Bruno et al. 2023). To the north is a tailed radio galaxy (extending E-W). The radio beam size is indicated in the bottom-left corner of each image. The contour levels are drawn at [1, 2, 4, 8. . . ] × 3σrms. Dashed contours depict the −3σrms contours. For MACS J0717+3745 image properties, see Table 4 (IM18 and IM19). The noise level of the LOFAR image of A2142 image is σ144 MHz = 400 μJy beam−1.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Zoom-in view of the MeerKAT UHF (top) and uGMRT Band 3 (bottom) 10″ resolution images, revealing substructures (marked with green curves) embedded in the northern part of the halo (K. Rajpurohit et al. 2025, in preparation). These features are identified in sensitive high-frequency observations but not detected in the less sensitive low-frequency images. When not masked, these features result in a second component at large radii in the radial profiles.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: A2744 full band continuum images of the central field from MeerKAT UHF (0.55–1 GHz) and uGMRT Band 4 (550–850 MHz) observations (in square-root scale). The figures show central halo emission and four relics in the outskirts (K. Rajpurohit et al. 2021b). Both images have a common resolution of 25″. The radio beam size is indicated in the bottom-left corner of each image. The contour levels are drawn at [1, 2, 4, 8. . . ] × 3σrms. Dashed contours depict the −3σrms contours. For image properties, see Table 4 (IM9 and IM10).
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Left: A2142 halo profiles extracted from the 75″  LOFAR HBA and LBA images. The average surface brightness is measured in circular annuli (see Figure 7 for used annuli). The solid lines show the best-fitting single-component exponential profiles.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: I0 − re plane at 1.4 GHz for the literature radio halos reported in M. Murgia et al. (2024) and those studied in this work. Dotted lines mark constant emissivities (in erg s−1 cm−3 Hz−1 units) obtained using Equation (2) assuming a redshift of z = 0.2 and α = −1 for reference.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Bullet cluster MeerKAT L band (0.9–1.7 GHz) and UHF (0.55–1.0 GHz) full band continuum radio images in square-root scale, showing a large scale central halo emission and a toothbrush-shaped relic to the east (S. P. Sikhosana et al. 2023). Both images have a common resolution of 15″. The radio beam size is indicated in the bottom-left corner of each image. The images show large scale asymmetrical halo emission. The contour levels are drawn at [1, 2, 4, 8. . . ] × 3σrms. Dashed contours depict the −3σrms contours. For image properties, see Table 4 (IM14 and IM15).
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Radial spectral index profiles of PLCK G287.0+32.9, A2744, and MACS J0717+3745. The error bars include flux scale uncertainties. To obtain these profiles, we measured average flux densities within concentric circular annuli from 50″  (PLCK G287.0+32.9), 25″  (A2744), and 20″  (MACS J0717+3745) resolution radio maps, with annulus widths of 50″, 30″, and 20″, respectively. All the observed spectral profiles of the halos show a radial steepening.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Top: Radial profiles extracted using circular, elliptical, and elliptical partial annuli. Profiles fitted with a single-component exponential model are shown with dashed lines. For the used annuli see Figure 7. Middle: Radial profiles using different sectors; the dashed line shows the fit to the combined profile from all sectors. Sectors are shown in Figure 14 right panel. Bottom: Radial profiles extracted using different choices of centers. The left panels show profiles extracted from an image where unrelated sources within the halo were masked out, while the right panels show profiles obtained from an image where unrelated sources were subtracted from the uv-data, as commonly used in the literature. The plot demonstrates that the selection of sectors, sector centers, and discrete source subtraction significantly impacts the extracted radial profiles in radio halos with large extents, potentially introducing an artificial, shallower, second component at larger radii.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Left: Sectors used to extract the PLCK G287.0+32.9 halo radial profiles shown in Figure  15 middle panels. Right: Different annuli centers (marked with “+” symbol and a circle of radius 10″) used to extract radial profiles shown in Figure  15, bottom panels. These sectors are overlaid on the 50″ MeerKAT UHF uv-subtracted point source image.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: NIRCam detected eYSC populations in M51 (left panel), M83 (top right panel), NGC 628 (middle right panel), and NGC 4449 (bottom right panel). For each galaxy, the RGB color scheme is the following: F335M continuum subtracted map (red), F187N continuum subtracted map (green), F115W map (blue). For NGC 628, we replaced F187N with F405N due to the better visual quality of the map. We highlight the position of the eYSC populations with black dots. In the three spiral galaxies, eYSCs are located along the spiral arms, where they are associated with the highest concentration of star-forming regions in the galactic disks.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Median values of the residual distributions mCIG − mobs (see Figure 5) for each available filter in eYSCI across the four galaxies studied in this work. For each panel, black crosses represent the corresponding median value of mCIG − mobs in that specific filter, for the entire population of eYSCI (where the total number of clusters is specified in the plot for each filter). HST filters present smaller numbers of clusters due to the additional S/N criteria we applied in this analysis. Different colors represent sub-samples of the population of eYSCI binned by the best-fitted age recovered with CIGALE. Additionally, we use two different symbols (square and triangle) to distinguish between two bins of masses (≤3000 M⊙, >3000 M⊙). For each data point, error bars correspond to the 16th–84th percentile of the residual distribution. Every galaxy in our sample exhibits an excess in the NIR, particularly more offset can be seen for the low mass and young (≤3 Myr) bins.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: NIR color–color diagrams in ABmag for simulated slug cluster libraries with different fixed stellar mass and color-coded by cluster age. The gray line represents a stellar evolutionary track computed with the yggdrasil code. Each point of the track is color-coded by age as the slug cluster libraries. For an observational comparison, we plotted median values and 16th–84th percentiles for the young cluster population in M51, NGC 628 and M83. We show the eYSCI populations with black symbols, while gray symbols represent the optically identified YSC populations younger than 10 Myr and with a fitted E(B − V) < 0.1, for a better comparison with the dust-free libraries. The extinction law vectors are from K. Fahrion & G. De Marchi (2023).
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Distributions of the residuals mCIG − mobs in eight selected filters (F555W, F814W, F115W, F150W, F187N, F200W, F300M, F444W) for the sample of eYSCI in M51. For each filter, mCIG − mobs represents the difference in magnitude between the best-fitted flux from the CIGALE fit and the observed flux, respectively. For each panel, we show the total number of eYSCI, which varies in HST filters due to the additional S/N requirements described in the text. To guide the reader’s eye, we plot a black vertical line at mCIG − mobs = 0.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Observed SEDs, best-fit models and recovered best fluxes for four representative eYSCs in M51. For each panel, the title of the plot describes the fitted properties of the specific eYSC (represented by a unique ID): ﹩{\chi }_{{\rm{reduced}}}^{2}﹩, age, and stellar mass. The observed fluxes in HST and JWST filters are shown with blue squares with error bars, while we show the CIGALE best-fitted fluxes convolved to each filter throughput with red filled circles. The black line represents the best model spectrum, while the remaining colored lines correspond to best-fitted models for the attenuated and unattenuated stellar component (orange and blue spectra, respectively), nebular (green spectrum), and dust emission (red spectrum). For each filter, we show the relative residual fluxes (obs - best)/obs in the lower portion of the panel.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Recovered ﹩{\chi }_{{\rm{reduced}}}^{2}﹩, Age, E(B − V), ﹩{U}_{{\rm{\min }}}﹩, γ and qPAH distributions from CIGALE for two different grids in M51. While the orange histograms show the results for the grid adopted in this paper (see Table 3), the blue distributions result from the empirically motivated dust grid (IF grid), as described in the text.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Normalized distributions of age, stellar mass, and E(B − V) for eYSCs in our sample of galaxies, obtained with CIGALE. We use different colors and line styles to distinguish the distributions of each galaxy. In the middle panel, we drew a dashed line at M* = 1000 M⊙ to guide the plot visualization. In the right panel, we added median values of the E(B − V) distributions as vertical lines.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Distribution of age differences for eYSCI in M51, M83, NGC 628, and NGC 4449, obtained using two different methods. For each panel, on the x-axis, AgeCIGALE represents the best-fit values of age from CIGALE, while AgeEW is estimated from Paα EWs, as described in Section 5.6. The unfilled histogram shows the entire population of eYSCI in the four FEAST galaxies, while we use filled histograms to compare the age differences using as a reference the CIGALE bin of ages defined in Section 4. Age bins are color-coded as in Figure 6.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Paα EW as a function of age for simulated slug cluster libraries with different fixed stellar masses of 500, 1000, 3000, 5000, and 10,000 M⊙, as defined in Section 5.4. Each panel corresponds to a specific stellar mass, as indicated by the label. The darker lines represent the median tracks of the simulated populations.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Median values of the residual distributions mCIG − mobs for eYSCI in M51, as shown in the top left panel of Figure 6. In this case, the CIGALE SED fit is performed up to the F200W filter and ignoring the contribution from the dust models.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Median values of the residual distributions mCIG − mobs for the optically selected YSC population in M51 younger than 10 Myr. The layout of the figure is as presented in Figure 6.