adsabs/AstroCLIMB huggingface dataset:
Paper: Precise Empirical Determination of Metallicity Dependence of Near-infrared Period–Luminosity Relations for RR Lyrae Variables
Authors: Anupam Bhardwaj, Marcella Marconi, Marina Rejkuba, Richard de Grijs, Harinder P. Singh, Vittorio F. Braga, Shashi Kanbur, Chow-Choong Ngeow, Vincenzo Ripepi, Giuseppe Bono, Giulia De Somma, Massimo Dall'Ora
Figure caption: Near-infrared PLRs for MW field RR Lyrae variables in the J (top), H (middle), and K  s  (bottom) bands. The solid black and dashed red lines represent the theoretical PLZ relations for [Fe/H] = −0.4 dex and −2.4 dex, respectively. The representative error bars on the left display ±3σ scatter in the theoretical relations (Marconi et al. 2015).
Paper: Precise Empirical Determination of Metallicity Dependence of Near-infrared Period–Luminosity Relations for RR Lyrae Variables
Authors: Anupam Bhardwaj, Marcella Marconi, Marina Rejkuba, Richard de Grijs, Harinder P. Singh, Vittorio F. Braga, Shashi Kanbur, Chow-Choong Ngeow, Vincenzo Ripepi, Giuseppe Bono, Giulia De Somma, Massimo Dall'Ora
Figure caption: Difference between the distance moduli (μ TW) resulting from Equation (1) and those from Baumgardt & Vasiliev (2021; μ GC), as listed in Table 1. The mean and the standard deviations of the residuals are quoted at the bottom left. The dashed and dotted lines represent the mean and 3 times the standard deviation of the residuals, respectively.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: CO (2–1) intensity as a function of mid-IR intensity at 1.″7 resolution. Individual points show individual lines of sight from our matched-resolution database with all four target galaxies plotted together. The points are colored by the mean extinction-corrected Hα intensity averaging all data within ±0.1 dex along each axis. Black and white points and error bars show the median and 16%–84% range in I CO after binning the data by mid-IR intensity. The red line shows the best-fitting power-law relation fit to the bins (Table 4) over the white region. Additional dotted lines indicate fixed I CO to mid-IR ratios. The white region shows our definition of “bright” emission (Section 3.4) while the gray-shaded regions are excluded from most statistical analyses either because we expect significant contamination by emission associated with non-CO-emitting gas (left region) or because only the starburst ring of NGC 1365 contributes data (right region). Each panel gives the slope (m) and intercept (b), and Table 4 gives the full numerical results. Figure 6 shows individual galaxy results.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR, CO, and extinction-corrected Hα maps for NGC 0628. These images show our matched 80 pc resolution, matched astrometry data for NGC 628. The top row shows two of the four analyzed JWST mid-IR images, F770W and F2100W. The bottom row shows the ALMA CO (2–1) image and the VLT/MUSE extinction-corrected Hα. All images are displayed using an identical arcsinh stretch from 0.5 to 30 MJy sr−1 after converting all bands to equivalent F770W using the band ratios in Table 1 for the mid-IR and the median ratios in Table 4 for CO (2–1) and Hα corr. We have blanked data outside the common JWST MIRI/MUSE/ALMA footprint. A scale bar shows 1 kpc at the distance of the galaxy and the 1.″7 (FWHM) beam appears in the top-right corner of the image. The blue contour in all panels shows an F770W contour at 1.5 MJy sr−1, and the red contour shows an Hα contour at an equivalent of F770W intensity 10 MJy sr−1.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR, CO, and extinction-corrected Hα maps for IC 5332. As Figure 1 but for IC 5332 at 70 pc resolution. Because the galaxy has a lower surface brightness than the other targets, the arcsinh stretch here runs from 0.25 to 5 MJy sr−1. All bands are expressed in equivalent F770W intensity, the blue shows an F770W contour now at a lower 0.5 MJy sr−1 and the red shows an Hα contour still at 10 MJy sr−1.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: CO (2–1) intensity as a function of mid-IR intensity at 1.″7 resolution, separated by galaxy. As Figure 5 but now showing the binned relation for each individual galaxy (colored points) along with a power-law fit to the binned data for each galaxy (colored lines). The dark gray-shaded curve indicates the 16%–84% range for the full data set, and the gray line indicates the same best-fitting power law for all data as shown in Figure 5. Each panel gives the slope (m) of the relationship, and Table 4 gives the full numerical fit values.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Extinction-corrected Hα intensity as a function of mid-IR intensity at 1.″7 resolution. As Figure 5 but now showing the relationship between extinction-corrected Hα intensity and mid-IR intensity with data points colored as in Figure 5 but now based on CO (2–1) intensity. The gray regions show the range of intensities excluded from statistical analysis and the red line shows the best-fitting power law describing the binned data for all galaxies. Each panel gives the slope (m) and intercept (b), and Table 4 gives numerical results. Figure 8 shows results for individual galaxies.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR, CO, and extinction-corrected Hα maps for NGC 1365. As Figure 1 but for NGC 1365 at 160 pc resolution. As in that figure, the arcsinh stretch runs from 0.5 to 30 MJy sr−1, and all bands are expressed in equivalent F770W intensity. As there, the blue shows an F770W contour at 1.5 MJy sr−1, and the red shows an Hα contour at equivalent to 10 MJy sr−1. Note the region blanked due to PSF effects at the galaxy center and also note that the bright region with I nu > 30 MJy sr−1 is excluded from most of our statistical analysis.
Paper: PHANGS–JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales
Authors: Adam K. Leroy, Karin Sandstrom, Erik Rosolowsky, Francesco Belfiore, Alberto D. Bolatto, Yixian Cao, Eric W. Koch, Eva Schinnerer, Ashley. T. Barnes, Ivana Bešlić, F. Bigiel, Guillermo A. Blanc, Jérémy Chastenet, Ness Mayker Chen, Mélanie Chevance, Ryan Chown, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Daizhong Liu, Laura A. Lopez, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Ismael Pessa, Jérôme Pety, Toshiki Saito, Amy Sardone, Jiayi Sun, David A. Thilker, Antonio Usero, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams
Figure caption: Mid-IR, CO, and extinction-corrected Hα maps for NGC 7496. As Figure 1 but for NGC 7496 at 150 pc resolution. As in that figure, the arcsinh stretch runs from 0.5 to 30 MJy sr−1, and all bands are expressed in equivalent F770W intensity. As there, the blue shows an F770W contour at 1.5 MJy sr−1, and the red shows an Hα contour at equivalent to 10 MJy sr−1. Note the region blanked due to PSF effects at the galaxy center.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: CMD F335M vs. F300M − F335M for NGC 7496. Magnitudes are in the AB system. In all panels, the black dots are F335M sources detected with Photutils find_peaks. Density contours for the densest parts of this diagram are shown in panels (a) and (b). In panel (a), yellow stars show the 12 prototype embedded clusters selected in our initial visual inspection. Based on the location in the CMD of these candidates, we select 67 embedded candidates (cyan circles). The dashed lines show the selection criteria: F300M − F335M > 0.3 and F335M < 24. The magenta box indicates a region where scatter due to the uncertainties in the color is large and is chosen for the purposes of illustrating the spatial distribution in Figure 5. Panel (b) shows the same extended sample of 67 candidates but differentiated by category: embedded (red), intermediate or partially embedded (green), and visible or exposed (blue). Panels (c) and (d) show for comparison the location in the CMD sources from the PHANGS-HST optical cluster catalog. Panel (c) shows clusters older than 100 Myr (magenta). As expected, these clusters fall around F300M − F335M = 0, indicating that these old sources do not have PAH emission. This panel also shows clusters with SED fit age estimates between 10 and 100 Myr (green plus signs) and 5–10 Myr (yellow diamonds), which also appear around F300M − F335M = 0. In contrast, about half of the clusters younger than 2 Myr shown in panel (d) (cyan crosses) are PAH emitters. Panel (d) also shows clusters between 2 and 5 Myr (orange squares), which mostly have little measured PAH emission.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: Left: combined HST F555W (blue) and JWST F335M (red) image. The green dots are sources detected in F335M that satisfy our color cut F300M − F335M > 0.3 (Section 3.3) but before performing any cut in magnitude. Sources shown in green without a magenta circle are the strongest PAH emitters and mostly found in the main dust lanes within the spiral arms. Sources with an additional magenta circle are those that have F300M − F335M between 0.3 and 0.7 and F335M > 24.5; i.e., they are both fainter and have larger color uncertainties (magenta box in Figure 2). This figure shows that when we select only the brightest sources with the largest color excesses, sources that tend to coincide with minor dust lanes in the galaxy, i.e., potentially fainter embedded clusters, are excluded. Middle: CO(2–1) ALMA map, with resolution of ∼1 with the 67 embedded cluster candidates (red circles). Right: MUSE Hα map with a resolution of ∼0.″7 and the 67 candidates. Note that the sample is well correlated with Hα and CO(2–1) peaks.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: The top panel shows the PHANGS-HST WFC3 F555M image of NGC 7496. The sample of 67 PHANGS–JWST 3.3 μm–selected star cluster candidates is plotted with different colors according to their categories: embedded (red), partially embedded (green), and visible (blue). The locations of optically selected clusters from the PHANGS-HST catalog are also shown and distinguished by SED fit age (black squares for >10 Myr and black circles for <10 Myr). Only clusters brighter than F300M < 25 are included. The bottom panels show images in the HST-WFC3, JWST-NIRCam, and JWST-MIRI filters for the 10″  ×  10″ region indicated by the white box in the top panel. The central wavelength of each filter is indicated in the panel label. The colored circles are the same as in the top panel. Clusters marked by an additional yellow circle are part of our prototype sample (see text for details). The comparison of this region in the optical HST images and IR from JWST clearly shows that the candidates fall along a dust lane, largely obscured in the HST bands.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: The LFs measured for different cluster samples are shown in the F200W (left) and F300M (right) filters. The red squares show distributions for the 67 dust-embedded cluster candidates from this work. The orange points show the LFs for PHANGS-HST–selected clusters at all ages (N = 263), and the blue dots are PHANGS-HST clusters younger than 10 Myr (N = 131). Green triangles indicate the LF of PHANGS-HST clusters plus the 67 embedded cluster candidates (N = 330). The green line shows the best-fit index to this last sample, while the orange line shows the fit for only the PHANGS-HST cluster distribution (orange circles). Our dust-embedded cluster sample (red squares) is not sufficiently deep to have many data points in the LF before the distribution begins to flatten, likely due to incompleteness, but by comparing the derived slopes with and without the embedded candidates, we observe that they are quite similar. The bright portion of each distribution appears to follow a trend that is consistent with that observed for the optically selected HST clusters. The upper axis indicates mass estimates from the method described in Section 4.2.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: Preliminary UV-IR SED of the 12 embedded prototype clusters (Section 3.1). Prototypes classified as partially embedded or “intermediate” are shown with dashed lines, and embedded clusters are shown as solid lines. For objects that are not detected in the HST bands, we show upper limits with gray arrows. These preliminary SEDs are constructed with fluxes measured with the same aperture in all bands, which leads to an underestimate of the flux in the MIRI bands and without aperture correction. Nevertheless, two features in the SEDs of embedded clusters are clearly seen: PAH emission at 3.3 μm and silicate absorption at 10 μm.
Paper: PHANGS–JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 μm PAH Emission
Authors: M. Jimena Rodríguez, Janice C. Lee, B. C. Whitmore, David A. Thilker, Daniel Maschmann, Rupali Chandar, Sinan Deger, Médéric Boquien, Daniel A. Dale, Kirsten L. Larson, Thomas G. Williams, Hwihyun Kim, Eva Schinnerer, Erik Rosolowsky, Adam K. Leroy, Eric Emsellem, Karin M. Sandstrom, J. M. Diederik Kruijssen, Kathryn Grasha, Elizabeth J. Watkins, Ashley. T. Barnes, Mattia C. Sormani, Jaeyeon Kim, Gagandeep S. Anand, Mélanie Chevance, F. Bigiel, Ralf S. Klessen, Hamid Hassani, Daizhong Liu, Christopher M. Faesi, Yixian Cao, Francesco Belfiore, Ismael Pessa, Kathryn Kreckel, Brent Groves, Jérôme Pety, Rémy Indebetouw, Oleg V. Egorov, Guillermo A. Blanc, Toshiki Saito, Annie Hughes
Figure caption: F200W magnitude vs. CI (measured as the difference in magnitude between circular apertures with 1 and 4 pixel radii). The vertical dashed line indicates CI =1.4, which can be used to distinguish clusters from stars (Whitmore et al. 2023, this volume). The colored circles represent our 67 cluster candidates as indicated; stars/point sources are represented by a star symbol. PHANGS-HST clusters younger than 2 Myr are small cyan small crosses, and those older than 100 Myr are small magenta triangles. The gray dots are all the sources detected in the F335M image.