adsabs/AstroCLIMB huggingface dataset:
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: Testing the link of the DFN to current star formation. Top: filament inclusion fractions for various star formation event tracers (H II regions, young clusters, young multiscale associations) vs. the dust emission filament extraction scale. Bars indicate results for each individual extraction scale, whereas lines and points indicate the cumulative filament mask measurements. Inclusion fractions for randomly distributed points are shown with inset bars and dotted lines. Bottom: SFR-weighted inclusion fractions.
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: Comparison of cumulative filament masks up to varied maximum scale. JWST  F770W image of NGC 628, overplotted with the contours showing the coverage of multiscale masks. The maximum scale is as follows: green, 100 pc; yellow, 140 pc; red, 200 pc; cyan, 280 pc; magenta, 400 pc. We adopt 200 pc as a preferred value. The scale bar corresponds to 1 kpc, 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: JWST  F2100W image with extracted emission filaments (cumulative up to 200 pc scale) shown as transparent colored areas. The image is 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: HST B-band (F435W) image with extracted attenuation filaments (25 pc scale) shown as transparent colored areas. The image is 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: JWST  F770W image with extracted emission filaments (cumulative up to 200 pc scale) shown as transparent colored areas. The image is 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: JWST  F2100W image with extracted emission filaments (35 pc scale) shown as transparent colored areas. The image is oriented north up and east left.
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: IC 5332 gas surface density from scaled F1130W emission. A single black contour highlights the brightness level where the F1130W emission implies Σgas = 7 M ⊙ pc−2. This figure and the subsequent figures for NGC 628, 1365, and 7496 (Figures 2, 3, and 4) are all shown with the same color bar. We show a 500 pc scale bar for reference.
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: Genus curves for the F1130W band, scaled to gas surface density (Equation (2)). The gray region shows where the noise dominates the statistic up to 3σ significance above the background, which corresponds to Σgas ≈ 2 M ⊙ pc−2. For a consistent comparison, we impose a radial cut at 0.4 R 25 in each galaxy, corresponding to 3.2, 5.7, 13.7, and 3.6 kpc in IC 5332, NGC 628, NGC 1365, and NGC 7496, respectively. The 11.3 μm emission traces a clear conversion from a “Swiss cheese” (genus < 0) to “meatball” topology (genus > 0) when going from low to high gas surface density.
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: Genus curves (top panels) from the gas surface density maps for two simulation snapshots (bottom panels). We show a gray vertical line at Σgas = 10 M ⊙ pc−2 as visual reference point to compare the two genus curves. The red contour indicates the surface density at the topology change measured by the genus zero crossing point. Left: M51-like simulation (Tress et al. 2020; Treß et al. 2021). Right: NGC628-like simulation (E. Emsellem et al. 2022, in preparation).
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: NGC 7496 gas surface density from scaled F1130W emission. A single black contour highlights the brightness level where the F1130W emission implies Σgas = 7 M ⊙ pc−2. In NGC 7496, saturation in the center leads to an artifact where the columns of pixels with saturation show low values. This is evident in the faint regions of our map.
Paper: GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114
Authors: J. Rich, S. Aalto, A. S. Evans, V. Charmandaris, G. C. Privon, T. Lai, H. Inami, S. Linden, L. Armus, T. Diaz-Santos, P. Appleton, L. Barcos-Muñoz, T. Böker, K. L. Larson, D. R. Law, M. A. Malkan, A. M. Medling, Y. Song, V. U, P. van der Werf, T. Bohn, M. J. I. Brown, L. Finnerty, C. Hayward, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, F. Muller-Sanchez, E. J. Murphy, D. Sanders, B. T. Soifer, S. Stierwalt, J. Surace
Figure caption: 2D images of the flux (a) and (d), relative velocity (b) and (e), and FWHM (c) and (f) generated from the spaxel-by-spaxel fits to the [Ne II] (12.8 μm) and H2 S(2) (12.3 μm) emission lines. The FWHMs shown are corrected for instrumental broadening as described in the text. The relative velocity map is generated by subtracting a systemic velocity of 6056 km s−1 from each spaxel. The broadest H2 FWHM in the NW is just outside the Channel 1 FOV but falls within the Channel 3 FOV, and corresponds to the eastern edge of the shocked “overlap” region observed in Saito et al. (2017). The elevated FWHM in [Ne II] is near apertures that show evidence of shocks and double peaked emission line profiles ((g), (h), (i), and (j)).
Paper: GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114
Authors: J. Rich, S. Aalto, A. S. Evans, V. Charmandaris, G. C. Privon, T. Lai, H. Inami, S. Linden, L. Armus, T. Diaz-Santos, P. Appleton, L. Barcos-Muñoz, T. Böker, K. L. Larson, D. R. Law, M. A. Malkan, A. M. Medling, Y. Song, V. U, P. van der Werf, T. Bohn, M. J. I. Brown, L. Finnerty, C. Hayward, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, F. Muller-Sanchez, E. J. Murphy, D. Sanders, B. T. Soifer, S. Stierwalt, J. Surace
Figure caption: Images and spectra of VV 114. Top left: Hubble Space Telescope (HST) 435W/814W color image. Middle left: JWST F770W image with the same FOV, where the green box corresponds to the MIRI SUB128 subarray FOV, as shown in the bottom left panel. Bottom left: F770W SUB128 image with MIRI MRS channel 1 FOV (dark blue Box), NIRSpec FOV (light blue box), and our ten 0.″4 radius extraction apertures. Right: full MIRI spectra of the 10 regions marked in the F770W subarray image. Spectra are shown at rest-frame wavelengths assuming a systemic velocity of 6056 km s−1 and sorted from top to bottom in order of decreasing 6.2 μm PAH EW.
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: NGC 1365 gas surface density from scaled F1130W emission. A single black contour highlights the brightness level where the F1130W emission implies Σgas = 7 M ⊙ pc−2. In NGC 1365, saturation in the center leads to an artifact where the columns of pixels with saturation show low values. This is evident in the faint regions of our map.
Paper: PHANGS–JWST First Results: Tracing the Diffuse Interstellar Medium with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies
Authors: Karin M. Sandstrom, Eric W. Koch, Adam K. Leroy, Erik Rosolowsky, Eric Emsellem, Rowan J. Smith, Oleg V. Egorov, Thomas G. Williams, Kirsten L. Larson, Janice C. Lee, Eva Schinnerer, David A. Thilker, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Daniel A. Dale, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Annie Hughes, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Laura A. Lopez, Daizhong Liu, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Miguel Querejeta, Toshiki Saito, Amy Sardone, Mattia C. Sormani, Jessica Sutter, Antonio Usero, Elizabeth J. Watkins
Figure caption: NGC 628 gas surface density from scaled F1130W emission. A single black contour highlights the brightness level where the F1130W emission implies Σgas = 7 M ⊙ pc−2.
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: HST  B band (F435W) image with extracted attenuation filaments (cumulative up to 200 pc scale) shown as transparent colored areas. The image is oriented north up and east left.
Paper: GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114
Authors: J. Rich, S. Aalto, A. S. Evans, V. Charmandaris, G. C. Privon, T. Lai, H. Inami, S. Linden, L. Armus, T. Diaz-Santos, P. Appleton, L. Barcos-Muñoz, T. Böker, K. L. Larson, D. R. Law, M. A. Malkan, A. M. Medling, Y. Song, V. U, P. van der Werf, T. Bohn, M. J. I. Brown, L. Finnerty, C. Hayward, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, F. Muller-Sanchez, E. J. Murphy, D. Sanders, B. T. Soifer, S. Stierwalt, J. Surace
Figure caption: NIRSpec spectra and PAH diagnostic plots used. (a) NIRSpec spectra of the NE and SW cores in VV 114. The SW core shows a strongly rising continuum characteristic of hot dust associated with an AGN. The 3.3 μm PAH feature is detected in both spectra, but is significantly weaker in the SW core. (b)–(c) Expanded region and fit to the 3.3 μm PAH feature in the NE (b) and SW (c) cores. (d) EW of the 6.2 μm PAH feature plotted vs. silicate strength. Measurements for our MIRI apertures are plotted as colored circles. Values measured with Spitzer/IRS for ULIRGs and LIRGs from the GOALS sample are plotted as “+” symbols, with VV 114E and three comparative ULIRGs denoted with red diamonds (Stierwalt et al. 2013). The starburst galaxy M82 is shown as a blue square (Spoon et al. 2007). (e) EWs of the 6.2 μm and 3.3 μm PAH features for the SW and NE cores (Inami et al. 2018). (f) Flux density ratio and 3.3 μm PAH EW for the SW and NE cores (Inami et al. 2018). The SW core lies near AGN-dominated ULIRGs in both diagnostic plots.
Paper: GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114
Authors: J. Rich, S. Aalto, A. S. Evans, V. Charmandaris, G. C. Privon, T. Lai, H. Inami, S. Linden, L. Armus, T. Diaz-Santos, P. Appleton, L. Barcos-Muñoz, T. Böker, K. L. Larson, D. R. Law, M. A. Malkan, A. M. Medling, Y. Song, V. U, P. van der Werf, T. Bohn, M. J. I. Brown, L. Finnerty, C. Hayward, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, F. Muller-Sanchez, E. J. Murphy, D. Sanders, B. T. Soifer, S. Stierwalt, J. Surace
Figure caption: Expanded view of spectral features present only in the NE nucleus (region (a)) indicative of a highly embedded source, compared with spectra of the SW nucleus (c) and region (f) (embedded cluster). The dashed vertical lines in each panel correspond to the following features. Top panel: absorption features due to aliphatic hydrocarbons at 6.85 and 7.25 μm. The spectra are normalized to 1 Jy at 6.7 μm. Middle panel: crystalline silicate absorption features at 16 and 19 μm combined with amorphous silicate absorption at 18 μm. The spectra are normalized to 1 Jy at 14.5 μm. Bottom panel: C2H2 and HCN absorption. The spectra are normalized to 1 Jy at 13.8 μm.
Paper: Inferring Type II-P Supernova Progenitor Masses from Plateau Luminosities
Authors: Brandon L. Barker, Evan P. O'Connor, Sean M. Couch
Figure caption: Iron-core mass (M Fe) distribution for the Sukhbold et al. (2016) progenitors up to 31 M ⊙. The horizontal dashed line represents a hypothetical 1.4 M ⊙ iron core with an uncertainty of 0.05 M ⊙ (shaded region). The blue circles represent ZAMS mass models that could, within the uncertainty, produce such an iron core.
Paper: Inferring Type II-P Supernova Progenitor Masses from Plateau Luminosities
Authors: Brandon L. Barker, Evan P. O'Connor, Sean M. Couch
Figure caption: The posterior distributions for ﹩{M}_{\min }﹩ and ﹩{M}_{\max }﹩ in units of M ⊙.
Paper: Inferring Type II-P Supernova Progenitor Masses from Plateau Luminosities
Authors: Brandon L. Barker, Evan P. O'Connor, Sean M. Couch
Figure caption: Left: iron-core mass distributions for the Sukhbold et al. (2016) progenitor set, convolved with the Salpeter IMF, for simulations that successfully produced explosions in STIR. Color indicates the ZAMS mass range of the progenitor in a bin. The unfilled black histogram represents the iron-core mass distribution for the G17 sample determined by our M Fe–L 50 fit. Bin widths for the inferred distribution are 0.03 M ⊙ to be comparable to iron-core mass uncertainties. Right: EDF for the inferred iron-core mass distribution of the G17 sample. The shaded regions represent the error region on the EDF due to the 68% uncertainties on the iron-core mass inferences. The dashed black line represents the iron-core mass where the primary contribution is from progenitors with ZAMS mass above 16.5 M ⊙, which is representative of the early Smartt (2015) result.
Paper: Inferring Type II-P Supernova Progenitor Masses from Plateau Luminosities
Authors: Brandon L. Barker, Evan P. O'Connor, Sean M. Couch
Figure caption: Distribution of observational plateau luminosities used in this work, taken from Gutiérrez et al. (2017a, 2017b).
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: The light-curve residuals for multiple bands (B, V, R, and T) after the PHOEBE model is subtracted.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: The observed radial velocities for J1527 as a function of the orbital phase obtained in 12 epochs from LAMOST, with the radial-velocity fit, plotted. The red velocity points are the radial velocities of the narrow H α  emission, which is in antiphase with the absorption-line velocities.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: The normalized B-, V-, R-band and TESS light curves for J1527 as a function of orbital phase. The black solid line represents the best-fitting model from PHOEBE.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: A set of panels showing the trajectory of J1527 around the Milky Way integrated backwards from the present day for 50 Myr.