adsabs/AstroCLIMB huggingface dataset:
Paper: Density Profiles of Collapsed Rotating Massive Stars Favor Long Gamma-Ray Bursts
Authors: Goni Halevi, Belinda Wu, Philipp Mösta, Ore Gottlieb, Alexander Tchekhovskoy, David R. Aguilera-Dena
Figure caption: Evolutions of the density and velocity profiles (in the top and bottom panels, respectively) of the M ZAMS = 18M ☉ and 13M ☉ models (left and right, respectively), during the GR1D evolutions through core collapse. The density profiles evolve similarly for both models, significantly flattening after the shock stalls. In the bottom left panel, there is infall within the core (at r < 106 cm) in the final snapshot for the 18M ☉ model, but there is no such infall in the final state of the 13M ☉ model. This is evidence that the core of the 18M ☉ model collapses to a BH at the end of its evolution, whereas the core of the 13M ☉ model remains a PNS.
Paper: PHANGS–JWST First Results: Duration of the Early Phase of Massive Star Formation in NGC 628
Authors: Jaeyeon Kim, Mélanie Chevance, J. M. Diederik Kruijssen, Ashley. T. Barnes, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Ralf S. Klessen, Kathryn Kreckel, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Steven N. Longmore, Sharon E. Meidt, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Erik Rosolowsky, Toshiki Saito, Karin Sandstrom, Eva Schinnerer, Rowan J. Smith, Antonio Usero, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: Top: comparison between the Spitzer 24 μm map (left) and the JWST 21 μm map (middle), which has 10 times better resolution (0.″67) compared to Spitzer (6″). Orange circles show the beam in each panel. Bottom: composite three-color images obtained by combining CO (blue), 21 μm (green), and Hα (red). The bottom right panel shows the zoomed-in image of the white rectangular region marked in the bottom left panel, with symbols indicating the distribution of emission peaks using the same color scheme. Emission peaks of CO (indicated with ×), 21 μm (+), and Hα (△) show spatial offsets, indicating that these represent distinctive stages of star formation. The JWST field of view is outlined in green. The crowded galactic center (white circle), as well as extremely bright star-forming regions (yellow circles) are excluded from our analysis (see text).
Paper: Density Profiles of Collapsed Rotating Massive Stars Favor Long Gamma-Ray Bursts
Authors: Goni Halevi, Belinda Wu, Philipp Mösta, Ore Gottlieb, Alexander Tchekhovskoy, David R. Aguilera-Dena
Figure caption: Stellar properties as functions of radius for the MESA models of AD20 at the onset of core collapse. In the four panels, we show (a) the mass density, (b) the temperature, (c) the radial velocity, and (d) the angular velocity. The different mass models are represented by the different colored and styled lines, as labeled, with the fiducial M ZAMS = 18M ☉ model being shown in solid magenta. We also include, with the dashed–dotted blue line, a fit to Equation (2) with α = 2.5, which represents the pre-collapse density profile that is characteristic of massive stellar progenitors and that has been ruled out by the observed properties of lGRBs (Gottlieb et al. 2022a). All models share similar density, temperature, and radial velocity profiles. Their core rotational velocities differ by factors of a few and vary nonmonotonically with the ZAMS mass.
Paper: PHANGS–JWST First Results: Duration of the Early Phase of Massive Star Formation in NGC 628
Authors: Jaeyeon Kim, Mélanie Chevance, J. M. Diederik Kruijssen, Ashley. T. Barnes, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Ralf S. Klessen, Kathryn Kreckel, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Steven N. Longmore, Sharon E. Meidt, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Erik Rosolowsky, Toshiki Saito, Karin Sandstrom, Eva Schinnerer, Rowan J. Smith, Antonio Usero, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: The top panel shows the flux contrast (﹩\delta {\mathrm{log}}_{10}{ \mathcal F }﹩) used to identify peaks on CO (blue) 21 μm (red) map as a function of the average filling factor ζ. The bottom panel shows the ratio of the feedback timescale (t fb,21 μm) and the total duration of the GMC life cycle (τ) as a function of ζ. In both panels, the shaded region shows the parameter space where crowding of sources can lead to an overestimation of the feedback timescale. Our data points are well outside of this region, confirming that we sufficiently resolve star-forming regions and our measurement of t fb,21 μm is reliable.
Paper: PHANGS–JWST First Results: Duration of the Early Phase of Massive Star Formation in NGC 628
Authors: Jaeyeon Kim, Mélanie Chevance, J. M. Diederik Kruijssen, Ashley. T. Barnes, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Ralf S. Klessen, Kathryn Kreckel, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Steven N. Longmore, Sharon E. Meidt, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Erik Rosolowsky, Toshiki Saito, Karin Sandstrom, Eva Schinnerer, Rowan J. Smith, Antonio Usero, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: Galaxy-wide SFR (SFRglobal) as a function of stellar mass (M *,global) for the PHANGS–JWST targets (circles), as well as nearby galaxies from (squares; Kim et al. 2021). For NGC 628 (this work) and nearby galaxies, the data points are colored by the duration of the embedded phase of star formation, derived using mid-infrared as an SFR tracer (t fb,MIR), which is JWST 21 μm for NGC  0628 and Spitzer 24 μm for other galaxies. The dashed line shows the star-forming main sequence of local galaxies (Leroy et al. 2019).
Paper: Discovery of a Dusty, Chemically Mature Companion to a z ∼ 4 Starburst Galaxy in JWST ERS Data
Authors: Bo Peng, Amit Vishwas, Gordon Stacey, Thomas Nikola, Cody Lamarche, Christopher Rooney, Catie Ball, Carl Ferkinhoff, Henrik Spoon
Figure caption: SED of SPT0418-47 system (red square) and the companion SE (blue square), along with the Arp-220 (red dashed line and red dotted line) and M82 (cyan dashed line) SED templates (Polletta et al. 2007) normalized by the dust continuum. The figure is adapted from Vishwas (2019).
Paper: XMM-Newton Detection of X-Ray Emission from the Metal-polluted White Dwarf G 29-38
Authors: S. Estrada-Dorado, M. A. Guerrero, J. A. Toalá, 宇君 杜, Y.-H. Chu, 有花 朱, V. Lora, C. Rodríguez-López
Figure caption: X-ray and optical/IR views of G 29-38. Top: ESAS EPIC X-ray composite picture in the 0.3–1.0 keV (red), 0.7–0.8 keV (green), and 1.0–2.0 keV (blue) energy bands. Middle: DSS red, blue and IR color-composite picture (1993 August 22) overimposed by the X-ray contours in the 0.7–0.8 keV (green) and 1.0–2.0 keV (cyan) bands. The red arrow shows the location of G 29-38 at the epoch of the XMM-Newton observation (2005.91). Bbottom: EPIC-pn event image with a solid circle showing the aperture used to extract the spectrum of G 29-38, and inner and outer dashed circles representing the circular aperture used to extract the spectra of the nearby source and the annular aperture used to extract a background spectrum suitable for G 9–38, respectively.
Paper: XMM-Newton Detection of X-Ray Emission from the Metal-polluted White Dwarf G 29-38
Authors: S. Estrada-Dorado, M. A. Guerrero, J. A. Toalá, 宇君 杜, Y.-H. Chu, 有花 朱, V. Lora, C. Rodríguez-López
Figure caption: Left: XMM-Newton EPIC-pn background-subtracted spectra (dots) of the source nearby to G 29-38. The black solid histogram represents the best fit to the data and the lower panel the residuals of the fit. Center: XMM-Newton EPIC-pn background-subtracted spectra (dots) of G 29-38 using distant background regions. The red-dashed histogram describes the contribution of the nearby source, whereas the gray histogram corresponds to the X-ray model of G 29-38 described by C2022. Right: XMM-Newton EPIC-pn background-subtracted spectra (dots) of G 29-38 using a background region around the nearby source. The black histogram is the optically thin isothermal (kT = 0.49 keV) vapec plasma X-ray emission model of G 29-38 with chemical abundances of the WD photosphere described by C2022. All spectra are binned to two counts per spectral bin.
Paper: XMM-Newton Detection of X-Ray Emission from the Metal-polluted White Dwarf G 29-38
Authors: S. Estrada-Dorado, M. A. Guerrero, J. A. Toalá, 宇君 杜, Y.-H. Chu, 有花 朱, V. Lora, C. Rodríguez-López
Figure caption: Cumulative frequency of the X-ray photons in the 0.4–1.2 keV energy range detected in the aperture of G 29-38. The dashed-line represents a constant X-ray flux.
Paper: XMM-Newton Detection of X-Ray Emission from the Metal-polluted White Dwarf G 29-38
Authors: S. Estrada-Dorado, M. A. Guerrero, J. A. Toalá, 宇君 杜, Y.-H. Chu, 有花 朱, V. Lora, C. Rodríguez-López
Figure caption: XMM-Newton EPIC-pn background-subtracted spectrum of G 29-38 with a bin width of 0.1 keV.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: NIR line identifications for SN 2021aefx; only the most dominant species for each feature are shown. We compare the JWST/NIRSpec spectrum of SN 2021aefx (black) at +255 days with a scaled GN/GNIRS spectrum of SN 2014J (red) at the closest available phase of +289 days (Diamond et al. 2018; Graur et al. 2020) and a scaled LBT/LUCIFER JHK s spectrum of SN 2011fe (blue) at a phase of +234 days (Mazzali et al. 2015). Nearly all emission lines are from significantly blended iron-group elements. The 2.5−5 μm region shows two strong blended features of predominantly [Fe III] 2.874 and 2.905 μm, and [Ni I] 3.120 μm and [Fe III] 3.229 μm, and several weak features. All spectra have been dereddened. Details of the NIR lines can be found in Table 2.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Combined optical + NIR + MIR spectrum of Type Ia SN 2021aefx in the nebular phase. The optical data are from SALT/RSS, and the NIR and MIR data were obtained with JWST/NIRSpec and JWST/MIRI, respectively. The optical flux is calibrated to ground-based photometry, and the MIRI flux is scaled to the MIRI F1000W photometry. The NIRSpec flux is unscaled from the JWST pipeline and matches up well to the optical and MIR. The spectrum has been dereddened and corrected for the host-galaxy redshift. For presentation purposes, the optical spectrum and the MIR spectrum past 12.5 μm have been rebinned to lower resolution. The flux axis uses a nonlinear (arcsinh) scale to better show all the features across a wide range of wavelength and F  ν . All subsequent spectra presented in the paper use a linear flux scale.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Optical line identifications for SN 2021aefx; only the most dominant species for each feature are shown. The optical spectrum (black) from SALT/RSS on 2022 August 7 at a rest-frame phase of +250 days is dominated by forbidden-line emission from iron-group elements. For comparison, we plot the JWST/NIRSpec spectrum (gray) on 2022 August 11 at +255 days, and the optical spectra of SN 2011fe (blue; Mazzali et al. 2015) and SN 2014J (red; Childress et al. 2015) at similar phase (+258 and +234 days, respectively). Phases are given with respect to B-band maximum, and all spectra have been dereddened.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: JWST MIRI F1000W verification image showing SN 2021aefx during target acquisition, before placement on the LRS slit. Part of the central region of the host galaxy, NGC 1566, can be seen in the bottom left corner; gas and dust features can be seen in the image on the right. Cosmic rays have been removed from the image.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: Contrasting filamentary dust structures in NGC 628 as seen in emission and attenuation, with emphasis on features identified at varied filament extraction scale. Top: JWST  F770W image. Dust emission filament mask boundaries are shown for 25 pc dashed, thin red; 200 pc, thick red; and cumulative 400 pc, dashed thin yellow. Bottom: B-band F435W HST  image, with attenuation filament mask coverage of 25 pc dashed, thin blue; 200 pc, thick blue. The scale bar in each panel is 1 kpc in length, and the images are oriented north up and east left.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: Filament overlap analysis for structures traced by visible attenuation and by MIR dust emission, as a function of extraction scale. Blue markings represent sight lines with attenuation only, magenta markings represent areas of overlap of between attenuation and emission, and red markings account for sight lines with emission only. Top: F770W. Bottom: F2100W. Results generated for cumulative masks are shown with points and sloping lines. We disregard scales >200 pc (shown faded in the plot) because the filament masks become unreliable (in the case of attenuation) or redundant with smaller-scale features (for emission). The first bar of the F770W plot (25 pc) presents the measurement for masks shown in Figure 1.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: Areal coverage of dust filaments. Top: for F770W, the fraction of pixels covered by a dust filament mask (emission or absorption) or left unassigned to a dust filament. Scales we elect to exclude from the filament network (see text) are shown faded in the plot. Bottom: same, for F2100W.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: A first comparison of dust filaments identified in absorption and emission. Left: preprocessed B-band HST  image, filtered to remove compact positive sources but retain small negative/concave morphological features. Center: filament masks for visible attenuation (blue) and MIR emission (red) extracted at a scale of 25 pc. Areas of overlap appear magenta. Right: JWST /MIRI F770W image. North is up, east is left, and the field of view spans 7.3 kpc from top to bottom. The figure only shows a portion of the area observed with JWST. The entire image may be seen in Figures 5 and A1–A4.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: Dust motes and point-source MIR contamination from extremely dusty stars. Left: subsection of our preprocessed B-band image, overlaid with contours corresponding to the filament masks generated at 25 pc resolution in emission, red, and absorption, blue. Center: unprocessed B-band image Right: JWST  F1000W image, also with the filament mask contours shown. Yellow circles surround three example dust motes. There are many more in the field shown, left unmarked. Green circles surround three example candidate dusty stars, others are not marked. Circles are 1″ in diameter, equivalent to 48 pc at the distance of NGC 628, and the images are oriented north up and east left.
Paper: PHANGS–JWST First Results: The Dust Filament Network of NGC 628 and Its Relation to Star Formation Activity
Authors: David A. Thilker, Janice C. Lee, Sinan Deger, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, Ralf S. Klessen, Eric Koch, J. M. Diederik Kruijssen, Adam K. Leroy, Ryan A. Lessing, Sharon E. Meidt, Francesca Pinna, Miguel Querejeta, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan J. Smith, Elizabeth J. Watkins, Thomas G. Williams, Gagandeep S. Anand, Francesco Belfiore, Guillermo A. Blanc, Rupali Chandar, Enrico Congiu, Eric Emsellem, Brent Groves, Kathryn Kreckel, Kirsten L. Larson, Daizhong Liu, Ismael Pessa, Bradley C. Whitmore
Figure caption: Measurements of the fraction of total flux contained within the DFN. Top: filament flux fraction in F770W expressed as percentage, with individual filament extraction scales plotted as pink bars and cumulative multiscale results as solid lines and points. The faded region is shown for completeness, although we adopt a maximum cumulative scale of 200 pc. Horizontal dashes on each bar indicate the 1σ uncertainty of the flux fraction measurements, obtained by perturbing the sky level in accordance with the postpipeline calibration described by Leroy et al. (2023, this Issue) and Lee et al. (Lee 2023, this Issue). Dotted lines show the 1σ range due to the uncertainty of cumulative flux fractions. Bottom: same, but for F2100W.