adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the disk masses obtained using the emitting heights from disksurf and those from DISCMINER.
Paper: An Actinide-boost Star Discovered in the Gaia-Sausage-Enceladus
Authors: Yangming Lin, Haining Li, Ruizheng Jiang, Wako Aoki, Satoshi Honda, Zhenyu He, Ruizhi Zhang, Zhuohan Li, Gang Zhao
Figure caption:  ﹩\mathrm{log}\epsilon ({\rm{Th}}/{\rm{Eu}})﹩ as a function of ﹩\left[{\rm{Fe}}/{\rm{H}}\right]﹩ for r-process-enhanced metal-poor stars. Circles represent ex situ stars, while triangles represent in situ stars. The red filled circles represent stars belonging to the GSE, while the blue filled circles denote stars from other substructures, including Wukong, Helmi streams, Thamnos, and Sequoia. The right Y-axis indicates the age calculated from ﹩\mathrm{log}\epsilon ({\rm{Th}}/{\rm{Eu}})﹩ (V. Hill et al. 2017). The black solid line corresponds to the actinide-boost criterion proposed by L. Mashonkina et al. (2014). Additionally, the black dashed line represents the age of the Universe (13.772 ± 0.059; C. L. Bennett et al. 2013). The references for the stellar data are compiled from V. M. Placco et al. (2023), supplemented by measurements from S. Honda et al. (2004), D. K. Lai et al. (2008), I. U. Roederer et al. (2009, 2010, 2018, 2024), C. M. Sakari et al. (2018), M. Hanke et al. (2020), D. Yong et al. (2021), M. Gull et al. (2021), P. Saraf et al. (2023), Q. Xing et al. (2024), and A. R. da Silva & R. Smiljanic (2025).
Paper: An Actinide-boost Star Discovered in the Gaia-Sausage-Enceladus
Authors: Yangming Lin, Haining Li, Ruizheng Jiang, Wako Aoki, Satoshi Honda, Zhenyu He, Ruizhi Zhang, Zhuohan Li, Gang Zhao
Figure caption: The abundance ratio of ﹩\mathrm{log}\epsilon ({\rm{X}}/{\rm{Zr}})﹩ for light neutron-capture elements and ﹩\mathrm{log}\epsilon ({\rm{X}}/{\rm{Sm}})﹩ for heavy neutron-capture elements as a function of ﹩\left[{\rm{Eu}}/{\rm{Fe}}\right]﹩. The gray dots represent the sample stars from I. U. Roederer et al. (2023). J0804+5740 is marked by a red pentagram. The solid black line shows the best fit obtained using the least-squares method (excluding J0804+5740), with the corresponding equation displayed at the bottom of each panel. The dashed black line indicates the baseline abundance calculated from stars with ﹩\left[{\rm{Eu}}/{\rm{Fe}}\right]\,\leqslant \,0.3﹩ in I. U. Roederer et al. (2023).
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Left panel: Emitting height as a function of radius for 12CO, assuming a disk mass of 0.01M⊙. We show the values from the DALI thermochemical model, as well as from our semianalytical model, for different values of the free parameter Nph. Central panel: Emitting height as a function of radius for 13CO, assuming a disk mass of 0.01M⊙ for different values of Nph. We compare the DALI data (black line) with the emitting layer predicted assuming Nph,13 = Nph,12 (blue line) and Nph,13 = Nph,1213C/12C (orange line). Right panel: Emitting height as a function of radius for 12CO, assuming a disk mass of 0.01M⊙ orbiting a Herbig star. We show the values from the DALI thermochemical model, as well as from our semianalytical model, for different values of the free parameter Nph.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Nτ, the CO column has τ = 2/3 for the J = 3–2 and J = 2–1 transition of 12CO and 13CO, as a function of temperature. The photodissociation column value we show is only a reference, and it will be estimated more precisely in Section 3.
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Surface density as a function of radius derived with the stratified model for LkCa 15. We show the results for both 12CO and 13CO; shaded regions show the uncertainties (see text for a discussion of the radial dependence of the uncertainty). For comparison, we also show the surface density implied by the fit to the rotation curve presented in this paper series in C. Longarini et al. (2025) and a constraint from optically thin C18O and C17O lines presented in J. A. Sturm et al. (2023).
Paper: exoALMA. XV. Interpreting the Height of CO Emission Layer
Authors: Giovanni P. Rosotti, Cristiano Longarini, Teresa Paneque-Carreño, Gianni Cataldi, Maria Galloway-Sprietsma, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Jochen Stadler, Richard Teague, Gaylor Wafflard- Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Like Figure 3, but for all the disks in our sample. We plot the constraint from the rotation curve (P. Martire et al. 2024; C. Longarini et al. 2025) as a dashed line when they only constitute upper limits. For the MAPS sample, the red line shows the surface density constraints from (partially) optically thin C18O (K. Zhang et al. 2021). Black dashed lines are visual aids showing r−1 and r−2 profiles.
Paper: The Ejection of Transient Jets in Swift J1727.8−1613 Revealed by Time-dependent Visibility Modeling
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, He-Xin Liu, Diego Altamirano, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Thomas D. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: VLBA images of the jets launched by Swift J1727.8−1613 on 2023 September 19. The first three panels show images of the 8.3 GHz observations with Gaussian tapers of increasing severity (as noted in the text boxes). The images are rotated counterclockwise by 90°, as shown by the compass in the top panel. The color bar shows the intensity in mJy/beam, and the contour levels are ﹩\pm \sigma \times {\sqrt{2}}^{n}﹩ mJy/beam where n = 3, 4, 5, . . . , and σ is the rms noise shown in the upper right of each image. The restoring beams of the images are shown by the ellipses in the bottom right of the panels. The images show a compact core and multiple downstream jet knots. The resolved jet knots are large and diffuse and are only detected with the shortest baselines. The bottom panel shows the simultaneous 2.3 GHz observation, which has lower sensitivity and poorer resolution. The distinct inner jet knots seen at 8.3 GHz are blended with the core at 2.3 GHz, but the downstream jet knot is clearly distinct and optically thin.
Paper: An Actinide-boost Star Discovered in the Gaia-Sausage-Enceladus
Authors: Yangming Lin, Haining Li, Ruizheng Jiang, Wako Aoki, Satoshi Honda, Zhenyu He, Ruizhi Zhang, Zhuohan Li, Gang Zhao
Figure caption: Top panel: the heavy-element abundance pattern for J0804+5740, compared with the solar r-process and s-process patterns (N. Prantzos et al. 2020; top left panel), as well as the theoretical r-process models combined with the asymptotic giant branch (AGB) s-process model (top right panel). The derived element abundances are depicted with red filled circles, with total error bars. Bottom panel: residuals between the derived element abundances and the solar r-process pattern (bottom left panel), as well as the theoretical r-process models combined with the AGB s-process model (bottom right panel) for J0804+5740.
Paper: The Ejection of Transient Jets in Swift J1727.8−1613 Revealed by Time-dependent Visibility Modeling
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, He-Xin Liu, Diego Altamirano, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Thomas D. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: Comparison of our analysis of the VLBA observation of Swift J1727.8−1613 using conventional imaging techniques and our dynamic model-fitting approach. The top panel shows the same image of Swift J1727.8−1613 as in the third panel of Figure 1, with the same rotation, color scale, and contours. The bottom panel shows a representation of our dynamic model fit, on the same scale. We plot the model using the median of the marginal posterior distribution for each fit parameter. The positions and sizes of the ellipses and circles show the evolution of the positions and FWHM sizes of the Gaussian components fit to the visibilities, where the colors of the components correspond to the time in hours from the reference time. The core component is shown in black since it is stationary and not changing in size. The downstream jet knots are moving away from the elliptical Gaussian core at varying speeds and are all expanding at different rates. An animated version of this figure is available in the Appendix.
Paper: The Ejection of Transient Jets in Swift J1727.8−1613 Revealed by Time-dependent Visibility Modeling
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, He-Xin Liu, Diego Altamirano, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Thomas D. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: MAXI/GSC light curves of Swift J1727.8−1613 during the beginning and flaring period of the outburst, with light curves and dynamic power spectra from HXMT in the LE (2–10 keV), ME (10–35 keV), and HE (27–250 keV) bands, surrounding the bright flare on 2023 September 19 (MJD 60206). The color scale of the dynamic power spectra shows the fractional rms normalized power. We note that we have adjusted the color scale to cut off the maximum power to highlight the fainter features. The horizontal lines show the 16th and 84th percentile credible interval estimations of the ejection dates of the three jet knots shown in Figure 2, corrected for the distance between the measured core position and the central black hole, estimated from the 2.3 to 8.3 GHz core shift. The ejection of the three jet knots is coincident with the bright X-ray flare and change in spectral and timing properties.
Paper: The Ejection of Transient Jets in Swift J1727.8−1613 Revealed by Time-dependent Visibility Modeling
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, He-Xin Liu, Diego Altamirano, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Thomas D. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: Constraints on the intrinsic jet speed and inclination for the three jet knots shown in Figure 2, using Equation (1), assuming a distance of 3.7 ± 0.3 kpc (D. Mata Sánchez et al. 2025). The lines use the median of the proper motion posteriors, the dark shaded regions include only the uncertainty in proper motion, while the light shaded regions also include the uncertainty in distance. This does not imply that knots 1 and 2 can be traveling at the same speed at the same inclination, since the knots must be at the same distance.
Paper: An Actinide-boost Star Discovered in the Gaia-Sausage-Enceladus
Authors: Yangming Lin, Haining Li, Ruizheng Jiang, Wako Aoki, Satoshi Honda, Zhenyu He, Ruizhi Zhang, Zhuohan Li, Gang Zhao
Figure caption: The spectral syntheses and the derived abundances for several key elements are presented. The black dots represent the observational spectrum. The red solid lines represent the best-fit syntheses, with an associated uncertainty of 0.2 dex (red shaded regions). The spectral syntheses excluding the elements of interest are shown as black dashed lines.
Paper: The Ejection of Transient Jets in Swift J1727.8−1613 Revealed by Time-dependent Visibility Modeling
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, He-Xin Liu, Diego Altamirano, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Thomas D. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: The fitted sizes of the downstream jet knots in our dynamic model of our 8.3 GHz VLBA observation of Swift J1727.8−1613. The red lines show the medians of the marginal posterior distributions, while the gray lines are 100 random samples from the posterior distribution. The three jet knots are different sizes and are apparently expanding at different rates.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: (a) F(4.65)/F(3.4) vs. F(3.4)/F(3.29), where F(4.65) is the power in the 4.65 μm aliphatic C–D feature, F(3.4) is the “clipped” estimate of the nonaromatic C–H stretch power, and F(3.29) is the “clipped” estimate of the aromatic C–H stretch power (see Figure 6). The right-hand scale shows the estimated (D/H)aliph. in the emitting nanoparticles, assuming K/f = 1.2. Deuteration is 2–3 times higher in M51 than in the Orion Bar. (D/H)aliph. does not appear to be correlated with the nonaromatic fraction. (b) Same as (a) but plotted against He+/H+. (D/H)aliph. appears to depend on the hardness of the radiation ionizing the H II region associated with the PDR where the PAHs are located.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: The 4.5–4.8 μm spectra of the four sight lines in Figure 2. Black curves: observed spectra. Dashed cyan curves: estimate for the dust-attenuated “continuum” (not including the 4.65 μm feature) but without absorption by ice or CO. Solid blue curves: continuum after absorption by ice and v = 0 CO. Green curves: continuum plus 4.65 μm emission feature (Equation (3)) with attenuation by dust, ice, and CO. Red curves: green curves plus emission lines of H, He, H2, v = 1 CO, and [K III] (see text). Inset profile: upper limit on an emission feature at 4.75 μm (see text).
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Comparison of the 3.1–3.65 μm emission in the different regions. The 3.29 μm feature profile is nearly invariant. The 3.37–3.60 μm emission shows regional variations in strength (relative to the 3.29 μm feature) and spectral details (see text). Dashed curves: Drude profiles for the 3.29 and 3.40 μm components (see text). The green shaded area shows the power included in ﹩{F}_{{\rm{arom.CH}}}^{\,{\rm{clip}}}﹩; the red shaded area shows the power in the Drude profile that is missed in ﹩{F}_{{\rm{arom.CH}}}^{\,{\rm{clip}}}﹩. We find ﹩{F}_{{\rm{arom.CH}}}^{\,{\rm{clip}}}/{F}_{{\rm{arom.CH}}}\approx 0.71﹩.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: The 4.2–4.6 μm spectra of the four sight lines in Figure 2. Black curves: observed spectra. Cyan dashed curves: estimate of continuum without ice absorption. Green curves: continuum with ice absorption applied. Red curves: continuum plus emission lines of H, He, and H2 (see text). The expected wavelengths for nitrile CN (∼4.35 μm) and aromatic C–D (∼4.40 μm) are indicated. In the M51 spectra, there is no evidence of nitrile CN emission or aromatic C–D emission; the inset profile shows our estimated upper limit on the strength of either feature.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: The 3–4 μm spectra of SW-Strip H II in M51 (left) and the “atomic PDR” in the Orion Bar (right). Red curve: model spectrum including emission lines. Areas shaded green and magenta show how the integrated intensities ﹩{F}_{{\rm{arom.CH}}}^{{\rm{clip}}}﹩ and ﹩{F}_{{\rm{nonarom.CH}}}^{{\rm{clip}}}﹩ are evaluated (see text).
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Selected recombination lines for NE-Strip H II. Black curves: observed spectrum. Red curves: model = continuum (green) + line emission. The differential extinction between 1.094 μm (Paγ) and 5.129 μm (Huδ) is consistent with the adopted K. D. Gordon et al. (2023) RV = 5.5 extinction curve and AV = 4.2 mag, with differential reddening A1.09 − A5.13 = 0.408AV = 1.71 mag determined to ±0.10 mag.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Same as Figure 7 but for two pointings in the Orion Bar (E. Peeters et al. 2024) and two positions in the M17 PDR (C. Boersma et al. 2023) (see text).
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Estimated extinction due to dust (dashed curves) and ices (red curves) over the 4–5 μm range for the four regions in M51 (see text).
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: Same as Figure 10 but for two positions in the Orion Bar (E. Peeters et al. 2024) and two positions in M17 (C. Boersma et al. 2023).