adsabs/AstroCLIMB huggingface dataset:
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Spatial localization errors of the TianQin EMRIs as a function of their eccentricities at the time of plunge. The gray (red) violin plots represent the probability distributions for the sky localization errors (D  L  estimation errors) of the EMRIs, and the gray (red) horizontal dashed line shows the median of the corresponding error.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Tesselation used for the spatially resolved spectral fitting analysis of the ACIS diffuse emission. Spectral fits to 11 sample extractions representing a range of locations and regions of interest (labeled in red and yellow in the soft diffuse image) illustrate the spectral complexity and diversity of the diffuse X-ray emission in 30 Dor. The outer boundary defines the “global” diffuse spectrum (Figure 10), plotted in the upper-left panel to facilitate comparison with the smaller extraction regions. Global and the other named regions outlined in red are based on SB contours: N157B and PWN (Figure 9), Manta Ray, Comet, and SE Ridge. The 308 tessellates (in green and yellow) come from the WVT Binning code by Diehl & Statler (2006).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Hubble Tarantula Treasury Project (HTTP) F160W image (Sabbi et al. 2013) showing the stellar content in the region of the Manta Ray diffuse extraction tesselate (blue outline). Three stellar overdensities are visible along the trailing edges of the Manta Ray “wings;” the one at lower right also shows NIR nebulosity suggesting an embedded cluster associated with the T-ReX point source c5160. The candidate X-ray pulsar (PSR J0538-6902 = T-ReX catalog source p1_799) is marked with a blue + sign enclosed by a red-blue ellipse showing the mask used to exclude the source from the diffuse emission. OB stars from the Very Large Telescope (VLT)-FLAMES Tarantula Survey (VFTS) catalog (Walborn et al. 2014; Evans et al. 2015) are marked with red + symbols with spectral types labeled; the majority are evolved massive stars. Extraction apertures for regular T-ReX catalog sources are outlined with blue polygons (occasional sources are omitted).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Diffuse X-ray spectra of N157B. (a) The N157B SNR spectrum with the central pulsar wind nebula (PWN) removed. (b) The J0537 PWN spectrum with the PSR J0537 point source removed. In these and other plots of spectral fitting presented below, the following parameters of various numbered models components are labeled: N H (absorbing hydrogen column density), kT (plasma temperature), tau (timescale), and SB (surface brightness, corrected for absorption N H).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: T-ReX event data (as in Figures 2 and 6) zoomed in to show the inner ∼35″ = 8.4 pc of the field, centered on the T-ReX aimpoint (R136). Events are binned by 0.5 sky pixels. Source positions are shown as blue diamonds for occasional sources and as white crosses for regular sources, with their ACIS source labels (Table 2; regular source labels in the most crowded central region are shown in black, with reduced size, for clarity). The piled-up W-R star Mk34 (p1_995) is noted in red.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: The global diffuse X-ray spectrum of 30 Dor, with the N157B SNR and its PWN removed. The “global” diffuse region is defined in Figure 11 below.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: The T-ReX event data with point-source extraction apertures overlaid, as in Figure 2, now zooming in on 30 Dor itself. Events are binned by 2 sky pixels.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Phase-dependent X-ray flux (top left) and median X-ray event energy (top right) for R144 (053853.36-690200.9, p1_1194, Doran916). Phase is calculated for a published optical period (74.2074 days) and T0 (periastron, MJD 58268.98; Shenar et al. 2021). A similar period estimate (∼74.4 days) was obtained from the X-ray data (bottom).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: 30 Dor diffuse emission in three soft X-ray bands. This is a zoom of Figure 3, cropped to a similar field as shown in Figure 6.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Phase-dependent X-ray flux (left) and median X-ray event energy (right) for R145 (053857.06-690605.6, p1_1256, VFTS695). The phase is calculated for a published optical period (158.76 days) and T0 (MJD 56022.6) (Schnurr et al. 2009; Shenar et al. 2017).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Phase-dependent X-ray flux (left) and median X-ray event energy (right) for R139 (053842.34-690458.1, p1_830, VFTS527). The phase is calculated for the period we estimate from the T-ReX data (∼153.0 days, bottom). T0 is derived from optical data (MJD 56041.3125, Hugues Sana, private communication).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: HD 269921 (053834.66-685306.1, pass52_4) light curve (blue, with grouped events in black) and median energy time series (red). Two complete “flare” events exhibit spectral hardening. Vertical dotted lines mark the boundaries of individual ObsIDs.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Flares within two single ObsIDs of foreground source 053935.54-690438.2 (p1_1521). Black + symbols depict the arrival time and energy of individual events, while the red curves give the cumulative distributions of arrival times. The p-values for the null hypothesis (constant flux) are 1 × 10−5 and 3 × 10−21 for ObsIDs 16202 and 16446, respectively.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: CAL69 (053816.28-692331.1, c4107) light curve, plotted with symbols and axes as in Figure 17. Frequent, low-amplitude flares are observed, with evidence for spectral hardening.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Phase modulation of the hot plasma absorption (left) and absorption-corrected luminosity (right) in a model of the R144 spectrum.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: The T-ReX event data for the full T-ReX field. Events are binned by 4 sky pixels (2″). Soft events (0.5–2 keV) are shown in red and hard events (2–7 keV) in green. Regular point sources are outlined by white polygons and “occasional” sources by blue polygons. Red polygons outline sources exhibiting significant pileup. These polygons are examples of event extraction regions, usually based on 90% encircled energy PSF contours. Notable off-axis sources discussed in the text are labeled in yellow.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: T-ReX diffuse emission in three soft X-ray bands, smoothed with adaptive kernels to achieve S/N = 15. All 3615 point sources (seen in Figure 2 above) were excised before smoothing. Axes are in celestial (J2000) coordinates.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: Light and shadow: zoomed and rescaled regions from Figure 4. These images illustrate the complex interfaces between the hot and cold ISM of 30 Dor. With respect to R136, these regions are located (a) northeast, (b) northwest, (c) southeast, and (d) southwest.
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: T-ReX diffuse emission in the Spitzer context. Spitzer images are from the Surveying the Agents of Galaxy Evolution (SAGE) survey (Meixner et al. 2006).
Paper: T-ReX: The Tarantula—Revealed by X-Rays
Authors: Leisa K. Townsley, Patrick S. Broos, Matthew S. Povich
Figure caption: ACIS exposure map with 2743 brighter (≥5 net counts) ACIS point sources overlaid; colors denote the median energy for each source. (a) The full T-ReX field. (b) A zoom of (a) showing the central ∼10′ of the ACIS field.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Modeled spectra of water rovibrational lines under different N tot, f  c , and b at R = 3500. All models have the same N beam (= f  c  N tot), and have the same line depths in particular in optically thin transitions, which are colored in gray shades and are indicated by gray arrows. Specifically, panel (a) shows that optically thin lines overlap regardless of the line width, b. Panel (b) shows that f  c  “dilutes” the spectral line depth. Panel (c) shows that, under the same N beam, if the product of b and f  c , bf  c , is also a constant, line profiles are indistinguishable, except for regions where optically thick lines overlap (e.g., at ∼5.214 μm, indicated by a magenta arrow). In such an overlapping region, a spectrum with a larger line width would have a smaller absorption intensity. Moreover, both panels (a) and (b) imply that larger bf  c  results in deeper optically thick lines.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Modeled water rovibrational spectra in three sets of N tot, f  c , and b at a spectral resolving power 3500. The physical conditions adopted in the model (a) follow the parameters derived from W3 IRS 5 used in Figure 1. In panels (b) and (c), the model in panel (a) is plotted in blue, and their differences with model (a) are plotted in red. The maximum difference and the corresponding standard deviation between the spectrum in (a) and (b) or (c) are labeled in the lower left of each panel. We note that the total column density in (b) and (c) differ by a factor of 50.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Modeled water rovibrational spectra at 10, 50, 100, 200, 500, 1000 K at a spectral resolving power of 3500. All models have the same total column density (N tot = 5 × 1018 cm−2), velocity width (b = 20 km s−1), and fractional coverage (f  c  = 1). We note that applying a different velocity width or a different fractional coverage would result in a similar spectral profile with different absorption depths (Figure 2). The R and the P branch are roughly located on the left and the right side of 11,0–10,1 and 10,1–11,0 labeled in the first panel. Specifically, a set of seemingly evenly spaced spectral lines in the R branch (marked with magenta ticks) that define the envelope of the spectrum stand out as T ex increases. These lines are composed of J 0,J –(J − 1)1,J−1 and J 1,J –(J − 1)0,J−1 transition when J ≥ 10 (see Figure 17(a) for detail).
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Flowchart illustrating our recommended process in interpreting MIR spectrum for unresolved lines, such as R ∼ 3000 for JWST. In this flowchart, yellow boxes represent analysis steps; green boxes represent parameters of interest; and gray boxes represent intermediate results of analysis. Compared to the “old method” where the whole spectrum is used for the χ 2 fitting to constrain bf  c , without knowing optically thick or thin lines (so as N beam), the new recipe is iterative for initial identification of optically thin and thick lines. Once optically thin lines are selected, N beam and T can be constrained via either the rotation diagram or curve-of-growth analysis, which are essentially the same for thin lines. Optically thick lines, with a good understanding of N beam, can then be used to constraint the product bf  c . Whether bf  c  can be decoupled depends on whether regions of optically thick and overlapping lines exist. Otherwise, one has to refer to external information, such as ground observational results, to decouple b and f  c .
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Modeled spectra of the ν 2 vibrational band of H2O of the massive protostar W3 IRS 5 observed by spectrometers on board SOFIA/EXES (R ∼ 50,000), JWST/MIRI (R ∼ 3500), and ISO/SWS (R ∼ 1500). The model assumes that a hot (T = 471 K) component with a water column density of ∼2.5 × 1019 cm−2 and a partial coverage of 40% is in front of W3 IRS 5. The right panels present zoomed-in modeled spectra from the red regions in the left panels. At the limited resolution of MIRI, often, many transitions blend into a broad, unresolved spectral structure.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: The comparison of the basic atmospheric stellar parameters (from left to right T eff, ﹩\mathrm{log}\,g﹩, and [Fe/H]) between the DD-PAYNE estimates and the DESI EDR catalog values from the SP pipeline. The color represents the number density of the stars. Here we only show stars with S/N > 20 and a good quality flag in both the DESI EDR and our measurements. The solid lines in the upper panels show the 1:1 line of the X- and Y-axes. The dotted lines in the upper middle panel indicate a T eff offset of ±400 K relative to the 1:1 line. Similarly, the dotted lines in the middle panel indicate a ﹩\mathrm{log}\,g﹩ offset of ±1.5 dex relative to the 1:1 line. In the right panels, the stars outside the dotted lines in T eff (upper left panel) and ﹩\mathrm{log}\,g﹩ (upper middle panel) are shown in gray. The mean and dispersion of the differences between DD-PAYNE and the DESI EDR parameters are marked in the figure. The number in brackets shows the dispersion after subtracting the systematic trend in the difference, as indicated by the violet line in the bottom panels.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Stellar number density distribution in the [Fe/H]–[Mg/Fe] plane for the DD-PAYNE results (left two panels) and the distribution in the [Fe/H]–[α/Fe] plane for the DESI EDR results from the SP pipeline (right two panels). The bottom panels are a column-normalized version of the top panels. Only stars with blue-band spectra S/N > 20 are shown in the figure.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Stellar number density distributions of the DESI EDR stars with blue-band spectra S/N > 10 in the T eff−﹩\mathrm{log}\,g﹩ diagram (left) and T eff−[Fe/H] plane (right). The stellar parameters in this figure are measured by the DD-PAYNE method. The S/N > 10 cut results in 249,877 stars being shown in each panel. The magenta line in the left panel shows the stellar isochrone for an age of 12 Gyr and [Fe/H] of −1.5, extracted from the PARSEC database (Bressan et al. 2012), while the red line shows the isochrone for an age of 4.0 Gyr and [Fe/H] of 0.0 (solar metallicity).
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Comparison of the differential spectrum for Mg between the DD-PAYNE prediction (red) and the Kurucz model calculation (gray) for a fiducial star, whose T eff, ﹩\mathrm{log}\,g﹩, [Fe/H], and [Mg/Fe] values are labeled in the figure. The zoomed-in plot highlights the Mg I B line region. The excellent match between DD-PAYNE and the Kurucz model in the differential spectrum ensures that the former determines the Mg abundance using physical features. These features are either directly the Mg lines or lines of other species affected by the opacity change due to the increase of the Mg abundance.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Comparisons of measurement errors in the DD-PAYNE stellar label estimates with the theoretical precision limit predicted by the CR lower bound. The top panel shows the case for a fiducial dwarf with T eff = 5900 K, ﹩\mathrm{log}\,g=4.0﹩, and [Fe/H] = −0.5 at a spectral S/N of 100. The lower panel shows the case for a giant star with T eff = 5000 K, ﹩\mathrm{log}\,g=2.5﹩, and [Fe/H] = −1.0 at a spectral S/N of 50. For T eff, the values on the vertical axis have units of 100 K. The bottom part of each panel shows the ratio between the DD-PAYNE results and the CR bounds.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Stellar number density distributions in the [X/Fe]–[Fe/H] abundance planes. Owing to the limitation of the training sample, different cuts at the lower-[Fe/H] ends are made for different elements. For N and Ti, a cut of [Fe/H] = −1.5 is taken, while a cut of [Fe/H] = −2.0 is taken for C, O, Al, Si, Ca, Cr, Mn, and Ni. For guidance, the red line shows the abundance trend of the dwarf stars in APOGEE DR17. For the majority of the elements, the stellar abundances from the DESI spectra are well consistent with the APOGEE DR17 trend.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Loss values as a function of epoch of the training process, for the 15th pixel of the spectra in our training sample, as an example. As shown in the legend, the gray curve shows the loss value contributed by the spectral flux of the training set, while the blue one shows the contribution of the regularization term from differential spectra. The black curve shows the loss value contributed by the spectral flux of the validation sample.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: Cross-validations of the labels with the test sample. In each panel, the medium value and the standard deviation between our estimates from DESI spectra and the LAMOST values are presented.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: The median of the correlation coefficients among the different labels, derived from the covariance matrix of the label fitting. The left and right panels are for the dwarfs and giants, respectively. The numbers in the figure mark the values of the correlation coefficients.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption: The distribution of the training stars in the T eff−﹩\mathrm{log}\,g﹩ diagram (left) and the [Fe/H]–[Mg/Fe] plane (right). The stars with red and blue dots are from APOGEE DR17 and LAMOST DR9, respectively.
Paper: Determining Stellar Elemental Abundances from DESI Spectra with the Data-driven Payne
Authors: Meng Zhang, Maosheng Xiang, Yuan-Sen Ting, Jiahui Wang, Haining Li, Hu Zou, Jundan Nie, Lanya Mou, Tianmin Wu, Yaqian Wu, Jifeng Liu
Figure caption:  T eff−﹩\mathrm{log}\,g﹩ distribution of the stellar grids for which the differential spectra are used to regularize DD-PAYNE in the current work. The T eff, ﹩\mathrm{log}\,g﹩, and [Fe/H] of these grids are drawn from the MIST isochrones (Choi et al. 2016). In total, there are 101 grids spanning [Fe/H] from −3 to 0.5. For each grid, 15 spectra are computed with the Kurucz ATLAS12 atmospheric model to provide the physical differential spectra for 15 labels.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Left: The ν 2 band transitions between J 0,J –(J − 1)1,J−1 and J 1,J –(J − 1)0,J−1. J 0,J –(J − 1)1,J−1 and J 1,J –(J − 1)0,J−1 lines overlap when J ≥ 9 and are separated when J < 9. These transitions in the R branch specifically consist of the envelope of the overall water spectral profile at ≳300 K. Right:  J 0,J –(J − 1)1,J−1 and J 1,J –(J − 1)0,J−1 transitions under different column density from 1017 to 5 × 1019 cm−2. Lines that are plotted are stronger than a detection limit of 1%.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Reference grids of line ratios under (N beam, T ex) with σ  v  = 2  km s−1 (b = 2.8 km s−1). The temperature axis is in an interval of 10 K, and the N beam axis is in an interval of 1017 (from 1017 to 1018 cm−2), 1018 (from 1018 to 1019 cm−2), and 1019 (from 1019 to 1020 cm−2).
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Modeled water rovibrational spectra similar to Figure 5 with N tot = 1 × 1019, 5 × 1019 cm−2.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Reference grids similar to those in Figure 18 with σ  v  = 100 km s−1.
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Reference grids similar to those in Figure 18 with σ  v  = 85  km s−1 (b = 120 km s−1).
Paper: On the Interpretation of Mid-infrared Absorption Lines of Gas-phase H2O as Observed by JWST/MIRI
Authors: Jialu Li, 佳璐 李, Adwin Boogert, Alexander G. G. M. Tielens
Figure caption: Reference grids similar to those in Figure 18 with σ  v  = 50  km s−1 (b = 70 km s−1).