adsabs/AstroCLIMB huggingface dataset:
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: CMDs showing ﹩{M}_{{K}_{s},0}﹩ absolute magnitude vs. ﹩{(J-{K}_{s})}_{0}﹩ color for Population I Hα-emission stars. The plotted quantities are corrected for interstellar absorption and reddening (Table 4). Symbols in the top panel represent spectral type: type M (circles), K (hexagons), G (squares), and F (triangles). Symbols in the lower panel depict luminosity class: luminosity class I or I–II supergiants (circles), and luminosity class II or III (squares). Open symbols in both panels show stars designated as post-AGB in Table 1. The dotted line in both panels corresponds to ﹩{M}_{{K}_{s},0}=-4.5﹩.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: CMDs showing (V − Ks) color in both panels vs. infrared ﹩{M}_{{K}_{s}}﹩ absolute magnitude (top panel) and visual MV absolute magnitude (lower panel) for the sample of Population I stars compiled for this study. Filled circles: stars known to exhibit strong Hα emission (Table 1). Open circles: stars not known to exhibit Hα emission. The dotted line corresponds to an absolute ﹩{M}_{{K}_{s}}﹩ magnitude of −4.5 mag. There is no correction for interstellar reddening or absorption.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: CMDs showing ﹩{(V-{K}_{s})}_{0}﹩ color (in both panels) vs. infrared ﹩{M}_{{K}_{s},0}﹩ absolute magnitude (top panel), and visual MV,0 absolute magnitude (lower panel) for the Population I stars known to exhibit Hα emission (Table 1). Data in both panels have been corrected for interstellar reddening (Table 4). Symbols in the two panels follow the convention of Figure 6. Those in the top panel represent spectral type: type M (circles), K (hexagons), G (squares), and F (triangles). Lower panel: class I or I–II supergiants (circles), and class II or III (squares). Open symbols represent post-AGB stars. Dotted lines correspond to an absolute ﹩{M}_{{K}_{s},0}﹩ magnitude of −4.5 mag.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: A DDO two-color diagram that shows C(45 − 48) vs. C(42 − 45) for stars in the Hα Population I compendium compiled for this work. Stars known to exhibit emission in the wings of the Hα line are shown as filled circles, whereas those not known to display such emission are depicted with open circles. Mean loci for luminosity classes V, III, and Ib are shown as solid lines, dotted lines, and dashed lines, respectively. Two panels are presented. In the top panel the data are the observed colors uncorrected for reddening (i.e., the data points for the Hαe stars are from Table 2). Only Hαe stars are shown in the bottom panel, again as filled circles, and the colors herein have been corrected according to the E(B − V) values listed in Table 4 and the reddening ratios noted in the text.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: The MV vs. (B − V) CMD for stars in the Population I Hα sample compiled for this study. Evolved stars known to exhibit emission in the blue and/or red wings of the Hα line on at least one occasion, i.e., those stars listed in Table 1, are shown as filled circles. Giants not known to exhibit such emission are depicted with open circles. There is no correction for interstellar reddening.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: The fields observed by the UKIRT team during the 2017 and 2018 seasons. The 2019 season contains the same regions except for the top row of orange grids. Each square represents a grouping of the four CCDs on WFCAM. The black area shows the 438 day overguide scenario for the Roman GBTDS fields (M. T. Penny et al. 2019; G. Zasowski et al. 2025). The background is the Milky Way as seen by the Gaia Data Release 3 using mw-plot (H. W. Leung 2023).
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Map of the ﹩{A}_{{K}_{S}}﹩ extinction of the Red Clump within the UKIRT field. This map uses the 2017 PSF photometry data with a ﹩{2}^{{\prime} }﹩ edge length. Each pixel on the map is therefore of size ﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩. The grayed region within ∣b∣ ≤ 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 and ∣l∣ ≤ 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 is where we only declare lower limits on the extinction. The gray shading sits behind the map and does not affect the color of the pixels themselves.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Shown are two example fields of stars that passed the quality cuts. The brown is a field close to the GC with significant extinction and reddening, whereas the orange is a field away from the Galactic plane where extinction and reddening have a lesser effect. The boxes enclose stars used in fitting the luminosity function to isolate the Red Clump outlined in Section 3.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption:  ﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩ map of the E(H − KS) reddening of the Red Clump using H- and KS-band UKIRT photometry. The grayed region within ∣b∣ ≤ 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 and ∣l∣ ≤ 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 denotes where we declare lower limits on the extinction. The gray shading sits behind the map and does not affect the color of the pixels.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: K-band filter used by the UKIRT microlensing survey as well as KS-band filters from VVV and 2MASS with transmission normalized to 1.0 for all filters. Filter profiles were provided by the Spanish Visual Observatory’s (SVO) Filter Profile Service (C. Rodrigo & E. Solano 2020).
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Mapping of the exponential gradient parameter, B, from our fits in UKIRT fields. We advise caution when using pixels with B < 0.2.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Illumination corrections for the 2017 UKIRT microlensing survey using the 2017 May and July products.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Same as in Figure 6 but for TOI-2046b. Below each flux plot, the residuals for the binned data are displayed with rms values of 0.51 mmag for TESS and 1.15 mmag for ADYU60.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Three new transit light curves of TOI-2046b observed with R (upper row) and V (lower row) filters on (left) 2021 December 17, (middle) 2023 July 3, and (right) 2023 August 5 with the T100 telescope.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Thirteen new transit light curves of TOI-2046b observed with the ADYU60 telescope.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Transit light curves of the exoplanet HAT-P-16b from two observational data sets. The left panel presents data from the TESS, and the right panel shows data from ADYU60. Each panel displays the normalized flux as a function of time, with unbinned data points shown as small black dots and binned data represented by a black line. The best-fit transit model is overlaid in red, highlighting the transit event. Below each flux plot, the residuals for the binned data are displayed with rms values of 0.58 mmag for TESS and 0.88 mmag for ADYU60.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: The left panel shows 11 new transit light curves of HAT-P-16b observed with the ADYU60 telescope along with the transit model fits indicated as red lines. The y-scale is arbitrarily adjusted to provide visual clarity. The right panel displays the residuals along with the dates (in the format: yyyymmdd) and the rms calculated from residuals (in mmag) for each light curve.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Same as in Figure 6 but for TOI-1516b. Below each flux plot, the residuals for the binned data are displayed with rms values of 0.33 mmag for TESS and 0.98 mmag for ADYU60.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Distribution of the RVs for HAT-P-16b in the top panel and the residuals in the bottom panel (L. A. Buchhave et al. 2010).
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Sixteen new transit light curves of TOI-1516b observed with the ADYU60 telescope.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: The plot of the target pixel files for TOI-1516 in sector 58 (top), TOI-2046 in sector 58 (middle), and HAT-P-16 in sector 17 (bottom). The black squares represent the chosen optimal photometric aperture utilized for the extraction of the SAP flux. It is important to note that the TESS pixel scale measures 21″.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Flowchart of the sensitivity calculation procedure.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: An example of a simulated εuniq = 0 event from the GSHM group, affected by the planet-binary degeneracy. Left panels show the grid search results projected onto the (h, k), (h, α), and ﹩(\mathrm{log}s,\mathrm{log}q)﹩ planes, with identified local minima labeled. The top right panel displays the full simulated light curve, and the middle right panels show a zoomed-in view of the anomalous region along with several selected optimized models and residuals relative to the 1L1S model. The bottom right panels present the source-lens trajectories and the caustic geometries for each selected model. Dashed circles indicate the source sizes, and the ﹩{\rm{\Delta }}{\chi }^{2}={\chi }^{2}-{\chi }_{{\rm{best}}}^{2}﹩ value for each model is labeled in “[ ]” brackets. In this case, Models (A, B), (C, D), (E, F), and (G, H) form close–wide degenerate pairs; thus, only the close models are shown for clarity. The central caustics of Models A and G are visually indistinguishable and are therefore shown together in one panel. Although models G, H, and I are excluded in this example due to their large Δχ2, they could survive under the conditions of lower effective cadence or lower SNR.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Same as Figure 3, but for an example εuniq = 0 event from the DSHM group that is affected by the planetary caustic close–wide degeneracy. Models A and B are visually indistinguishable on the grid search plots but represent different geometries.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: The α-integrated sensitivity maps εanom (without accounting for 2L1S degeneracy), ε (with 2L1S degeneracy included), and their difference for the DSHM group. The white dots indicate the actual sampled points in the simulation, and the full map is linearly interpolated in the (k, h) space. The upper panels show the complete maps, and the lower ones provide zoomed-in views of the boxed region, where k and h are defined in Equations (2) and (3).
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Left: the ﹩(\alpha ,\mathrm{log}s)﹩-integrated sensitivities εanom (solid lines) and ε (dashed lines) as a function of ﹩\mathrm{log}q﹩ for all event groups. Right: the relative decrease in sensitivity after accounting for εuniq for all groups.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Left and middle: the α-integrated sensitivity difference maps for the DSHM group under default (left) and denser (middle) sampling grids. The close–wide degenerate pair from the event in Figure 4 is marked with star symbols connected by a dashed line. Right: relative decrease in ﹩(\alpha ,\mathrm{log}s)﹩-integrated sensitivity as a function of ﹩\mathrm{log}q﹩ for the default (solid black) and denser (dashed red) sampling grids.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Same as Figure 3, but for an example εuniq = 0 event from the DSEM group that was affected by the central-resonant degeneracy.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: Estimated decrease in the sample planetary sensitivity of a microlensing survey (for example, KMTNet, S.-L. Kim et al. 2016) due to 2L1S degeneracy, as a function of the planet-host mass ratio q.
Paper: Binary-lens Microlensing Degeneracy: Impact on Planetary Sensitivity and Mass-ratio Function
Authors: Yuxin Shang, 钰欣 尚, Hongjing Yang, 弘靖 杨, Jiyuan Zhang, 纪元 张, Shude Mao, 淑德 毛, Andrew Gould, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Jennifer C. Yee
Figure caption: The SNR curve used in the light-curve generation, obtained from applying the Q. Qian et al. (2025) pipeline to the KMTNet-SAAO 2018 observations.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Distribution of the RVs for TOI-1516b in the top panel and the residuals in the bottom panel (P. Kabáth et al. 2022).
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Timing residuals of HAT-P-16 b with future projections of the three transit-timing models shown with 150 random draws from the MCMC posterior chains. Each data point is the difference between an observed time and the time predicted by the best-fit constant-period model. The size of the data points corresponds to the data quality index from 1 to 3, with the higher-quality transits being larger. The red crosses represent observations removed during the sigma-clipping process.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Distribution of the RVs for TOI-2046b in the top panel and the residuals in the bottom panel (P. Kabáth et al. 2022).
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Timing residuals of TOI-2046b with future projections of the three transit-timing models shown with 150 random draws from the MCMC posterior chains. Each data point is the difference between an observed time and the time predicted by the best-fit constant-period model. The size of the data points corresponds to the data quality index from 1 to 3, with the higher-quality transits being larger. The red crosses represent observations removed during the sigma-clipping process.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: The GLS periodogram of HAT-P-16b. The top panel displays the power spectrum, the middle panel (left) shows the TTV distribution of the system, the bottom panel (left) presents the residuals, the middle panel (right) illustrates the variation of periodicity with phase, and the bottom panel (right) shows the residuals from the fit.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: Timing residuals of TOI-1516b with future projections of the three transit-timing models shown with 150 random draws from the MCMC posterior chains. Each data point is the difference between an observed time and the time predicted by the best-fit constant-period model. The size of the data points corresponds to the data quality index from 1 to 3, with the higher-quality transits being larger. The red crosses represent observations removed during the sigma-clipping process.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: The GLS periodogram of TOI-2046b. The top panel displays the power spectrum, the middle panel (left) shows the TTV distribution of the system, the bottom panel (left) presents the residuals, the middle panel (right) illustrates the variation of periodicity with phase, and the bottom panel (right) shows the residuals from the fit.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: The GLS periodogram of TOI-1516b. The top panel displays the power spectrum, the middle panel (left) shows the TTV distribution of the system, the bottom panel (left) presents the residuals, the middle panel (right) illustrates the variation of periodicity with phase, and the bottom panel (right) shows the residuals from the fit.
Paper: A Combined TESS and Ground-based Study of Transit Timing Variations in HAT-P-16, TOI-1516 and TOI-2046 Systems
Authors: E. Sonbas, K. Kaplan, M. Tanriver, A. Keskin, K. Dhuga, A. Bulut, E. Göğüş, W. Ogłoza
Figure caption: FAP values for each system.
Paper: Measuring Interstellar Carbon Abundance via 158 μm [C II] Absorption with SOFIA—A Potential Detection and Proof-of-concept for Depletion Studies with Future Far-IR Facilities
Authors: Christopher J. R. Clark, Julia. C. Roman-Duval, Suzanne C. Madden, Marc Mertens, Claire E. Murray, Jürgen Stutzki, Elizabeth Tarantino, Kirill Tchernyshyov
Figure caption: SOFIA-upGREAT 157.7 μm spectrum of the IC 342 sightline, plotted in blue. Plotted in orange is a model of dust continuum plus Gaussian [C II] emission from IC 342 itself, produced by fitting only to data outside the Milky Way velocity range. This model has significant residuals, shown in purple, centered around vLSR ∼ 0 km s−1. Also shown for reference, in black, is the HI4PI 21 cm H I spectrum with Tb × 0.03, for ease of comparison with the [C II] data. The −90 ≳ vLSR ≳ + 15 km s−1 Milky Way H I velocity range is shaded in green. The 21 cm spectrum exhibits HI emission associated with IC 342 at +20 ≳ vLSR ≳ + 120 km s−1.
Paper: Measuring Interstellar Carbon Abundance via 158 μm [C II] Absorption with SOFIA—A Potential Detection and Proof-of-concept for Depletion Studies with Future Far-IR Facilities
Authors: Christopher J. R. Clark, Julia. C. Roman-Duval, Suzanne C. Madden, Marc Mertens, Claire E. Murray, Jürgen Stutzki, Elizabeth Tarantino, Kirill Tchernyshyov
Figure caption: Idealized model spectra for the sightline toward background galaxy NGC 7331. Left panel: predicted model of 158 μm continuum emission from NGC 7331 with Milky Way [C II] absorption; also plotted is the predicted MW [C II] emission, and the observed Milky Way H I emission (from HI4PI) for reference. Central panel: predicted combined spectra of background galaxy continuum emission plus Milky Way [C II] emission, plotted with and without absorption from Milky Way [C II]. Right panel: same as center panel, but with data binned to the 3 km s−1 velocity resolution of the Far-InfraRed Spectroscopy Space Telescope (FIRSST; see Section 5.2), with Gaussian noise added to match the level expected from integration to per-channel S/N = 10, to simulate observed spectra. Also plotted is the continuum + [C II] absorption spectrum after the Milky Way [C II] is subtracted.