adsabs/AstroCLIMB huggingface dataset:
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: The BPT diagram of our sample. This includes all the galaxies used in our four methods.
Paper: Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks
Authors: Byeongseon Park, Alexander Pitňa, Jana Šafránková, Zdeněk Němeček
Figure caption: Correlations between transition range spectral index ﹩{\alpha }_{{\rm{tr}}}﹩ and turbulence parameters estimated over 10 minute intervals. (a) ﹩{\alpha }_{{\rm{tr}}}﹩ vs. the absolute value of normalized cross helicity ∣σc∣, (b) ﹩{\alpha }_{{\rm{tr}}}﹩ vs. normalized fluctuation amplitude σB, and (c) ﹩{\alpha }_{{\rm{tr}}}﹩ vs. bulk speed ∣V∣. Dots and vertical bars indicate medians and their error; horizontal dashed lines show parameter medians and interquartiles. (d) Radial trends of ∣σc∣ and σB for FF shocks (upstream: black/green; downstream: red/blue). (e) Corresponding trend in ﹩{\alpha }_{{\rm{tr}}}﹩. Data are drawn from SolO, PSP, and Wind FF shock sets.
Paper: Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks
Authors: Byeongseon Park, Alexander Pitňa, Jana Šafránková, Zdeněk Němeček
Figure caption: Statistical evolution of normalized spectral index ﹩{\alpha }_{\mathrm{tr}}/{\langle {\alpha }_{\mathrm{tr}}\rangle }_{10\,\,\rm{minutes}\,}﹩ and ﹩{\rm{\Delta }}\alpha {\rm{tr}}﹩ across FF and FR shocks. (a)–(b) Results from SolO and PSP FF shocks; (c)–(d) Wind FF shocks; (e)–(f) Wind FR shocks. In all panels, medians (black lines or dots) and their errors (red bars) are shown. Histograms display distributions of ﹩{\rm{\Delta }}{\alpha }_{{\rm{tr}}}^{{\rm{up}}}﹩ (blue), ﹩{\rm{\Delta }}{\alpha }_{{\rm{tr}}}^{{\rm{md}}}﹩ (green), and ﹩{\rm{\Delta }}{\alpha }_{{\rm{tr}}}^{{\rm{dn}}}﹩ (red). For clarity in visualization, we limit the display range to ﹩| {\rm{\Delta }}{\alpha }_{{\rm{tr}}}^{{\rm{ud}}}| \lt 2.5﹩, while values exceeding this threshold are represented as a fraction of the total number of ﹩{\rm{\Delta }}{\alpha }_{{\rm{tr}}}^{{\rm{ud}}}﹩. The time for FR shocks is flipped for consistency: negative (positive) times correspond to upstream (downstream).
Paper: The Sulfur Plume in the Horsehead Nebula: New Detections of S2H, SH+, and CO+
Authors: A. Fuente, G. Esplugues, P. Rivière-Marichalar, D. Navarro-Almaida, R. Martín-Doménech, G. M. Muñoz-Caro, A. Sánchez-Monge, A. Taillard, H. Carrascosa, J. J. Miranzo-Pastor, A. Tasa-Chaveli, P. Fernández-Ruiz, V. V. Guzmán, J. R. Goicoechea, M. Gerin, J. Pety
Figure caption: Zero-moment images of the H2S 1(1,0)→1(0,1), S2H 14(1,14)→13(0,13), SO2 4(2,2)→3(1,3), CO+ N = 2→1, J = 5/2→3/2 , SO+ J = 15/2→13/2, Ω = 1/2, l = e, and SH+ N = 0→1, J = 1→0, F = 3/2→1/2 lines. The H2S line is taken from A. Fuente et al. (2017). Units are in K km s−1 for H2S and Jy beam−1 × MHz for the ALMA maps presented in this work. In colors, we indicate the regions selected to extract the spectra shown in Figure 2. The beam is drawn in the bottom left corner. Two contours of the H2S 1(1,0)→1(0,1) are drawn in all panels for reference. Green, yellow, pink, and white squares corrrespond to Mol-peak, Sulfur-plune, IF, and IF2, respectively (see text).
Paper: The Sulfur Plume in the Horsehead Nebula: New Detections of S2H, SH+, and CO+
Authors: A. Fuente, G. Esplugues, P. Rivière-Marichalar, D. Navarro-Almaida, R. Martín-Doménech, G. M. Muñoz-Caro, A. Sánchez-Monge, A. Taillard, H. Carrascosa, J. J. Miranzo-Pastor, A. Tasa-Chaveli, P. Fernández-Ruiz, V. V. Guzmán, J. R. Goicoechea, M. Gerin, J. Pety
Figure caption: Averaged spectra of the H2S 2(2,0)→2(1,1), S2H 14(1,14)→13(0,13), SO2 4(2,2)→3(1,3), CO+ N = 2→1, J = 5/2→3/2 , SO+ J = 15/2→13/2, Ω = 1/2, l = e, and SH+ N = 0→1, J = 1→0, F = 3/2→1/2 lines in the areas defined in Figure 1.
Paper: The Sulfur Plume in the Horsehead Nebula: New Detections of S2H, SH+, and CO+
Authors: A. Fuente, G. Esplugues, P. Rivière-Marichalar, D. Navarro-Almaida, R. Martín-Doménech, G. M. Muñoz-Caro, A. Sánchez-Monge, A. Taillard, H. Carrascosa, J. J. Miranzo-Pastor, A. Tasa-Chaveli, P. Fernández-Ruiz, V. V. Guzmán, J. R. Goicoechea, M. Gerin, J. Pety
Figure caption: The N(CO+)/N(SH+) ratio as a function of visual extinction as predicted by the Meudon PDR code using the parameters shown in Table A3. Different colors correspond to different values of the sulfur elemental abundance: S/H = 1.5 × 10−5 (red), S/H = 1.5 × 10−6 (blue), and S/H = 1.5 × 10−7 (black). Solid and dashed lines correspond to the G0 = 60 and 186 Mathis field, respectively. The blue band indicates values of N(CO+)/N(SH+) = 0.08−0.30, consistent with our observations toward the IF assuming an uncertainty of a factor of ∼2. Only S/H > 1.5 × 10−6 can fit our estimations.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Color–color and color–magnitude diagrams for sources in JWST/NIRCam images of NGC 2024 (black points and red circles), members of IC 348 with types of ≥L0 (red points), and TWA 27B (cross). The latter is shown in only the top diagram. The red line is a reddening vector used for selecting the ≥L0 candidates in NGC 2024.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Histograms of extinction-corrected absolute magnitudes in H or F162M (left) and [4.5] or F444W (right) for known members of IC 348 in our IMF sample (solid line) and the remaining viable NIRCam candidates that lack spectroscopy (dotted line).
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: IMF for an extinction-limited sample of members of IC 348 within the NIRCam field (points) and the mass function after including the remaining viable candidates from NIRCam that lack spectroscopy (open circles). The latter points are shifted slightly in mass for clarity.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: JWST/NIRSpec spectra for two brown dwarf candidates in IC 348 and a filler target that are active galaxies.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Photometry in F162M and F444W vs. the equivalent width of the 3.4 μm feature for brown dwarfs in IC 348 (Figure 7). Error bars are omitted when they are smaller than the symbols.
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: The MZR measured using the four metallicity indicators and a comparison with others. Solid dots in the left panel represent measurements from individual sources, while the black dashed lines indicate the best-fit results. The gray shade around best-fit model represents the error. Data points are color-coded with the redshift of galaxies. In the right panel, the solid points in various colors and the corresponding solid lines represent the individual source measurements and their best-fit models for each method, just the same as the left panel. The dashed green and orange lines indicate the MZR provided by R. L. Sanders et al. (2021) at redshifts of 2.3 and 3.3. The translucent gray points represent the results with MaNGA using N2S2Hα (C. Ma et al. 2024).
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: The relative scatter in residual ﹩\mathrm{log}({\rm{O}}/{\rm{H}})﹩, denoted as ﹩\sigma /{\sigma }_{{\rm{\min }}}﹩, as a function of β. Solid lines in different colors show results obtained using various metallicity indicators. The pink shaded region represents the best-fit β range for redshifts z = 0–5 from the TNG50 simulations. The green shaded region marks the 1σ range around the best-fit β in MaNGA using the N2S2Hα indicator. Data for both TNG50 and MaNGA are taken from C. Ma et al. (2024).
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Correlation between ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩ and ﹩{\rm{\Delta }}\mathrm{log}{R}_{{\rm{e}}}﹩. Solid circular points represent individual galaxies, color-coded by redshift. Green diamonds indicate the median values within three bins: (−3σdZ, −σdZ), (−σdZ, σdZ), and (σdZ, 3σdZ). The Spearman rank p-values are displayed in the upper-left corner of each panel.
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: The redshift–stellar mass diagram of our sample. Sky-blue and pink points represent star-forming galaxies and AGNs, respectively, from the final samples used for different metallicity measurement methods. Gray dots indicate all galaxies in the JADES field with available stellar mass and photometric redshift measurements.
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Similar to Figure 3, but showing a comparison between our results and those from local observations and simulations. Blue dots represent our measurements using the N2S2Hα indicator. In the left panel, the blue contour and gray points show results from MaNGA (C. Ma et al. 2024). In the right panel, colored contours represent TNG simulation results across different redshift slices.
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: The mass-extinction diagram for galaxies with O3Hβ measurements. Sky-blue points represent sources classified as star-forming galaxies, while pink points indicate sources identified as AGNs. Green points correspond to potential AGN candidates. The solid and dashed red lines show the high- and low-probability AGN classification thresholds from S. Juneau et al. (2014), respectively. In this work, we adopt the solid red line as our selection criterion.
Paper: Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks
Authors: Byeongseon Park, Alexander Pitňa, Jana Šafránková, Zdeněk Němeček
Figure caption: Example of FF IP shock observed by SolO on 2023 February 21. (a) Magnetic field magnitude, (b) proton bulk speed, and (c) proton density and differential ion energy flux. (d) Illustration of 1 minute sliding computation intervals in upstream (subscript “u”) and downstream (subscript “d”) within ±85 s of the shock passage. Blue (red) shaded regions mark the nearest upstream (downstream) interval. (e) Magnetic field spectra for 10 minute intervals at up- and downstream, including the MAG instrument transition range noise floor (see green solid and dashed lines). Gray dashed lines with asterisks indicate the fitted slopes with spectral breaks. (f) A full set of power spectra within ±10 minutes of the shock crossing.
Paper: Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS
Authors: Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi, András Pál
Figure caption: Top panel: Maxwellian mode frequency of the suspected C-type population as a function of the fraction of this population among Hildas. The solid curve corresponds to a fast-rotator (P ≤4 hr) fraction of 1% in the whole population. The gray-shaded region marks the region corresponding to the 0.8%–1.2% C-type fraction curves. The vertical dashed line marks the C-type fraction obtained by R. Gil-Hutton & A. Brunini (2008). Bottom panel: SDSS (g − r) and (r − i) colors and their uncertainties for (42237) (black cross) and (207644) (orange cross). The rectangles with labels mark the approximate areas of the main taxonomy types C, D, and S (blue, purple, and red, respectively), as defined by A. V. Sergeyev & B. Carry (2021).
Paper: Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks
Authors: Byeongseon Park, Alexander Pitňa, Jana Šafránková, Zdeněk Němeček
Figure caption: Evolution of turbulence parameters across a FR shock observed by Wind on 2003 May 30. (a) Magnetic field power spectra over ±10 minutes. (b) Temporal evolution of ﹩{\alpha }_{{\rm{tr}}}﹩; the shaded region denotes 2σ from ﹩{\langle {\alpha }_{\mathrm{tr}}\rangle }_{10\,\mathrm{minutes}}﹩. (c) Change in spectral index, ﹩{\rm{\Delta }}{\alpha }_{{\rm{tr}}}﹩. (d) Normalized cross helicity, ∣σc∣, and (e) fluctuation amplitude, σB. Negative (positive) times indicate downstream (upstream) due to the spacecraft-frame geometry for FR shocks with a subscript “dn” (“up”). Magenta vertical lines mark the shock crossing, and yellow-shaded intervals around t = 0 are excluded from statistical analysis.
Paper: Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS
Authors: Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi, András Pál
Figure caption: Rotational properties of inner solar system asteroids. The top panel shows rotational frequency vs. absolute magnitude, with the dashed horizontal line marking the rotational breakup limit (a 2.2 hr period) from P. Pravec & A. W. Harris (2000). The bottom panel plots light-curve amplitude against rotational frequency, with dashed curves indicating constant critical densities from P. Pravec & A. W. Harris (2000). In both panels, different colors represent data from various sources, as shown in the legend. The three asteroids studied in this Letter are highlighted with filled yellow circles, and the two fast rotators from K2 are marked with filled pink circles. The filled blue circles indicate the fast-rotating Trojans from C. Kiss et al. (2025).
Paper: Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS
Authors: Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi, András Pál
Figure caption: Folded light curves and rotational frequencies for the three fast-rotating Hilda asteroids. Top panel: light curves are folded with the obtained rotation periods, also listed in Table 1. The gray points, representing the observations, are binned with 24, 26, and 22 bins for asteroids (42237), (91273), and (237321), respectively. Middle panel: power spectra with the false alarm probabilities (FAP) marked with dashed lines. Bottom panel: light curves obtained from the ZTF survey and folded with periods, indicated on the figures.
Paper: Three Fast-spinning Medium-sized Hilda Asteroids Uncovered by TESS
Authors: Nóra Takács, Csaba Kiss, Róbert Szakáts, Emese Plachy, Csilla E. Kalup, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, Róbert Szabó, Attila Bódi, András Pál
Figure caption: Cohesion vs. density curves for our targets obtained using the Drucker–Prager criterion of failure. The colors correspond to the following targets: black—(42237); red—(91273); orange—(237321); purple—(207644); blue—(208290). Dashed and solid curves correspond to friction angles of ϕ = 40° and 45°, respectively.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: JWST/NIRSpec spectra collected in this work and in L24 for brown dwarfs in IC 348. The first four objects are normal young L dwarfs. The remaining sources exhibit the 3.4 μm feature from an unidentified aliphatic hydrocarbon. The wavelength range of that feature is marked by the pink band. For reference, the central wavelength of the Q branch of CH4 (not detected in these objects) is indicated by the blue tick mark. Two brown dwarfs (LRL 2296 and LRL 11040) have large excess emission at >3.5 μm and absorption features that may arise from ices (H2O, CO2, OCN−, CO). For each spectrum that has been shifted upward, the level for zero flux is marked by a pair of dotted tick marks.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Color–color and color–magnitude diagrams for point sources in NIRCam images of IC 348 from Cycle 3. We have marked the previously known members that are not saturated and the candidate members identified with these diagrams, some of which have been classified as new members, field T dwarfs, or galaxies with NIRSpec (Table 2). The criteria used for selecting candidates are indicated (solid lines).
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: JWST/NIRCam images of two close pairs in IC 348. LRL 1546 is a previously known brown dwarf, while LRL 11043 and LRL 11044 are classified as new brown dwarfs with NIRSpec (Figure 7). LRL 11056 lacks spectroscopy, but its colors are consistent with a late spectral type. The size of each image is 1″ × 1″. North is up and east is left.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Proper motions measured for point sources in JWST/NIRCam images of IC 348 from Cycles 1 and 3. We have marked the six previously known members of the cluster that appear in both epochs and are not saturated, three of which were discovered with the Cycle 1 data. We also indicate the proper motion of the cluster based on Gaia DR3.
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: m162 vs. the median difference between 2 and 4 pixel aperture photometry among the available bands for sources in NIRCam images of IC 348 from Cycle 3. This metric is used to classify the sources as pointlike (<0.1) or extended (≥0.1).
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: JWST/NIRSpec spectra for brown dwarf candidates in IC 348 that are background T dwarfs (left) and highly reddened background stars that were selected as filler targets (right).
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: Map of the known members of IC 348 prior to this work and the fields imaged by JWST/NIRCam in Cycles 1 and 3 (inner and outer rectangles).
Paper: A New Spectral Class of Brown Dwarfs at the Bottom of the IMF in IC 348
Authors: K. L. Luhman, C. Alves de Oliveira
Figure caption: JWST/NIRCam images in three filters (F162M, F360M, and F444W) from Cycle 3 for a ﹩16^{\prime} \times 20^{\prime} ﹩ field in IC 348.
Paper: HDO Ice Detected toward an Isolated Low-mass Protostar with JWST
Authors: Katerina Slavicinska, Łukasz Tychoniec, María Gabriela Navarro, Ewine F. van Dishoeck, John J. Tobin, Martijn L. van Gelder, Yuan Chen, A. C. Adwin Boogert, W. Blake Drechsler, Henrik Beuther, Alessio Caratti o Garatti, S. Thomas Megeath, Pamela Klaassen, Leslie W. Looney, Patrick J. Kavanagh, Nashanty G. C. Brunken, Patrick Sheehan, William J. Fischer
Figure caption: NIRSpec spectra of L1527 from 3.7 to 4.2 μm extracted with 1″ apertures from the region where the flux at 5 μm is maximized (top panel, black line) and the region where ice absorption features are still present but the CO2 scattering wing is minimized (middle panel, purple line). The dashed red lines indicate the local continua fit to these spectral regions, and the insets show the respective extracted regions in the NIRSpec data cube. The bottom panel compares the extracted optical depth spectra resulting from these local continuum fits to the two spectra. The local continuum in the top panel was used to calculate the optical depth spectrum presented in Figure 2.
Paper: HDO Ice Detected toward an Isolated Low-mass Protostar with JWST
Authors: Katerina Slavicinska, Łukasz Tychoniec, María Gabriela Navarro, Ewine F. van Dishoeck, John J. Tobin, Martijn L. van Gelder, Yuan Chen, A. C. Adwin Boogert, W. Blake Drechsler, Henrik Beuther, Alessio Caratti o Garatti, S. Thomas Megeath, Pamela Klaassen, Leslie W. Looney, Patrick J. Kavanagh, Nashanty G. C. Brunken, Patrick Sheehan, William J. Fischer
Figure caption: Silicate-subtracted NIRSpec (top) and MIRI (bottom) spectra of L1527 on the optical depth scale (solid black line) along with the fit components for H2O ice: amorphous H2O at 40 K (dashed–dotted blue line), amorphous H2O at 80 K (solid purple line), crystalline H2O at 80 K (dotted magenta line), and the total combined ice fit (dashed light blue line). The observational data between 8.7 and 11.7 μm have been smoothed with a 10-point boxcar average to ameliorate the higher noise level due to the deep silicate feature at these wavelengths. Peaks of other major species (e.g., CO2, CO) are labeled in gray but not fit. The temperatures indicated in this figure should not be interpreted as the extracted physical temperatures of the observed H2O ice (see Sections 2.2.2 and 3.2). See Figure B2 for the global continuum fit and Figure B3 for the silicate subtraction.
Paper: HDO Ice Detected toward an Isolated Low-mass Protostar with JWST
Authors: Katerina Slavicinska, Łukasz Tychoniec, María Gabriela Navarro, Ewine F. van Dishoeck, John J. Tobin, Martijn L. van Gelder, Yuan Chen, A. C. Adwin Boogert, W. Blake Drechsler, Henrik Beuther, Alessio Caratti o Garatti, S. Thomas Megeath, Pamela Klaassen, Leslie W. Looney, Patrick J. Kavanagh, Nashanty G. C. Brunken, Patrick Sheehan, William J. Fischer
Figure caption: NIRSpec spectrum of L1527 on the optical depth scale from 3.7 to 4.2 μm (solid black line) along with the ice fit components CH3OH (dashed–dotted brown line), a Gaussian representing SH-bearing ices (dotted yellow line), amorphous HDO (solid blue line), crystalline HDO (solid magenta line), and the total combined ice fit (dashed green line). The gray horizontal shaded region indicates the 3σ noise level. See Figure B1 for the local continuum used to extract this spectrum.