adsabs/AstroCLIMB huggingface dataset:
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: MIRI spectrum of L1527 on the optical depth scale following global continuum subtraction (solid black line) along with the silicate fit components pyroxene (dashed–dotted gray line) and olivine (dotted lime line) and the total combined silicate fit (dashed green line). This silicate fit was used to isolate the 12 μm H2O ice libration feature shown in Figure 3. 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.
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: Global continuum fit to the combined NIRSpec and MIRI spectrum of L1527 across the 2.5–27.9 μm spectral range. 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. The dashed red line shows the polynomial continuum used to perform the global continuum subtraction, while the translucent purple line shows how the profile of this polynomial can be reproduced with two blackbody emission profiles, one at 453 K (dotted red line) and another at 104 K (dotted blue line).
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: The 5 μm continuum maps from the L1527 data cubes collected via NIRSpec IFU G395M (top) and MIRI-MRS (bottom) with the positions of the respective 1″ and 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩30 diameter apertures used to extract the analyzed spectra shown in white.
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: Comparison of HDO/H2O ratios measured in various primitive solar system objects and toward protostars in both ices and the gas phase. The ice HDO/H2O ratio of L1527 measured in this work using JWST data is indicated with the large orange hexagon. The data and their sources can be found in Tables F1 and F2.
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: Comparison of absorption bands from the same ice species at NIRSpec and MIRI wavelengths. Top left: the 4.39 μm 13CO2 stretching mode (NIRSpec). Top right: the 15.2 μm 12CO2 bending mode (MIRI). In both top plots, the red dashed lines mark peak positions indicating the presence of pure CO2 ice that segregated from other ice species during thermal processing. Bottom left: fit to the 3.53 μm CH3OH C–H stretching mode (NIRSpec). The gray lines indicate the optical depth of this spectral region extracted with the upper- and lower-limit continua shown in Figure D3. Bottom right: fit to the 9.7 μm CH3OH C–O stretching mode (MIRI) using the same combination of CH3OH laboratory data used to fit the 3.5 μm complex in the bottom left panel. The data were binned using a binning factor of 30 to reduce the noise levels due to the CH3OH band being located at the tip of the nearly saturated silicate feature. The black line indicates the optical depth of this spectral region after the silicate subtraction shown in Figure B3. The gray line indicates the optical depth of this spectral region extracted using the local continuum fitting procedure described in Section 2.1 of S. Bottinelli et al. (2010).
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: Optical depth of the 9.7 μm silicate feature plotted as a function of H2O ice column density toward low-mass protostars. The blue data points were obtained from Spitzer data (A. C. Boogert et al. 2008), and the blue dashed line shows the best linear fit to the data. The red diamond represents L1527 using the H2O ice column density from Y. Aikawa et al. (2012), while the golden hexagon represents L1527 using the H2O ice column density from this work. Both L1527 data points use the silicate optical depth obtained from the MIRI spectrum in this paper.
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: The local continua and subsequent fits to the 3.7–4.2 μm region used to define continuum uncertainties on the HDO column densities. First row: the lower (left) and upper (right) limits on the local continua in the central spectrum. Second row: the corresponding lower (left) and upper (right) limits on the local continua in the off-source spectrum. Third row: comparisons of the extracted spectra resulting from the lower- (left) and upper- (right) limit continua between the two positions. Fourth row: ice fits to the spectra extracted using the continua in the first row. The resulting HDO column densities were used to define the HDO column density uncertainty from the continuum choice.
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: The local continua and subsequent fits to the 3.3–3.7 μm region used to define continuum uncertainties on the CH3OH column densities. Top row: the lower (left) and upper (right) limits on the local continua in the central spectrum. Bottom row: ice fits to the spectra extracted using the continua in the top row. The resulting CH3OH column densities were used to define the CH3OH column density uncertainty from the continuum choice.
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 3.3 to 3.7 μm (solid black line) along with the ice fit components of pure CH3OH (solid brown line), a 1:5 CH3OH:H2O ice mixture (dashed–dotted blue line), a Gaussian representing NH3 hydrates or NH4+ salts (dotted lavender line), and the total combined ice fit (dashed green line). This CH3OH fit was used to constrain the contribution of CH3OH to the 3.7–4.2 μm region shown in Figure 2. See Figure B4 for the local continuum used to extract this spectrum.
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: Local continuum fit to the 3.3–3.7 μm spectral region used to extract the optical depth spectra in Figure B5.
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: The global continua and subsequent silicate subtractions and H2O ice fits used to define continuum uncertainties on the H2O column densities. First row: the lower (left) and upper (right) limits on the global continua in the central spectrum. Second row: the silicate subtraction performed on the optical-depth-scale spectra extracted using the continua in the top row. Third and fourth rows: H2O ice fits to the NIRSpec and silicate-subtracted MIRI spectra. The resulting H2O column densities were used to define the H2O column density uncertainty from the continuum choice.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: A comparison of the 2D correlation plots between ∑mν (eV) and various other parameters across various data combinations.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: A comparison of the 1D marginalized posterior distributions for ∑mν (eV) across various data combinations. The panel on the right shows results with the DES Year 1 WL included. Note that in the right panel, the Planck PR4+lensing+DESI2+DESY5+WL data set combination leads to a 2σ+ detection of nonzero ∑mν. The two vertical black dashed lines (in both panels) indicate the minimum mass thresholds for the normal (0.057 eV) and inverted (0.096 eV) neutrino mass hierarchies, respectively.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: 68% and 95% marginalized contours in the w0,DE–wa,DE plane for different data combinations. The area to the right of the vertical dashed blue line and above the slanted dashed blue line represents the parameter space corresponding to quintessence-like or non-phantom DE.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: A comparison of the 1D marginalized posterior distributions for Ωm and S8 across various data combinations. Note that the Ωm posteriors remain similar with the addition of WL data, but the S8 values are lowered.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: The left and middle panels show the 1D posterior distributions of Neff and H0 (km s−1 Mpc−1), respectively, for various data combinations. The dashed vertical line in the left panel corresponds to the standard model value of Neff = 3.044. The right panel shows the 2D correlation plot between the two parameters, showing a strong correlation between them.
Paper: Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly
Authors: Shouvik Roy Choudhury
Figure caption: The top panel shows the 1D posterior distributions of Alens for various data combinations. The bottom panel shows its 2D correlation plots with the S8 parameter. We note that data set combinations with WL included leads to a 2σ+ lensing anomaly due to the strong correlation with S8.
Paper: Where Have All the Little Red Dots Gone? Supermassive Black Hole Binary Dynamics and Its Impact on Galaxy Properties
Authors: Fazeel Mahmood Khan, Benjamin L. Davis, Andrea Valerio Macciò, Kelly Holley-Bockelmann
Figure caption: SMBH binary parameters for our galaxy merger study with five different simulation runs. Top-left panel: separation of the pair of SMBHs as the galaxies merge during the initial phase of their runs. Top-right panel: the complete evolution of the separation between SMBHs as they pair and merge, driven by dynamical friction, three-body scattering, and gravitational-wave emission. Bottom-left panel: the inverse semimajor axis of each SMBH binary system as a function of time. Bottom-right panel: the eccentricity evolution of the SMBH binaries.
Paper: Where Have All the Little Red Dots Gone? Supermassive Black Hole Binary Dynamics and Its Impact on Galaxy Properties
Authors: Fazeel Mahmood Khan, Benjamin L. Davis, Andrea Valerio Macciò, Kelly Holley-Bockelmann
Figure caption: Initial volume density (ρ) profiles of our galaxy models (top panel) and surface stellar density (Σ⋆) profiles of the same (bottom panel).
Paper: Where Have All the Little Red Dots Gone? Supermassive Black Hole Binary Dynamics and Its Impact on Galaxy Properties
Authors: Fazeel Mahmood Khan, Benjamin L. Davis, Andrea Valerio Macciò, Kelly Holley-Bockelmann
Figure caption: Time/redshift evolution of half-mass radii and surface densities within the half-mass–radius for our various models. The dotted lines always represent the evolution following the GW kick. Top: time (T) evolution of the half-mass radii (R1/2) of the newly formed galaxies resulting from mergers. The half-mass radii increase as the SMBHs scour the central regions of their coalesced host galaxies and deposit mass into larger radii. M0 is our stability run, and we witness that the half-mass radii at T ∼ 100 Myr remain practically unchanged. The filled teal circle (A. C. Carnall et al. 2023) and orange star (A. de Graaff et al. 2024) symbols depict the observed half-light radii for quiescent galaxies with masses similar to those used for our simulations. Bottom: the surface density within the half-mass–radius (﹩{{\rm{\Sigma }}}_{{R}_{1/2}}﹩) plotted as a function of time.
Paper: Where Have All the Little Red Dots Gone? Supermassive Black Hole Binary Dynamics and Its Impact on Galaxy Properties
Authors: Fazeel Mahmood Khan, Benjamin L. Davis, Andrea Valerio Macciò, Kelly Holley-Bockelmann
Figure caption: Evolution of galaxy profiles in merger products (from the top to bottom rows: M1, M2, M3, M4, and M5) across the times of binary formation, hard binary formation, and gravitational-wave-dominated phases at the time of SMBH coalescence. Profiles include cumulative mass (left column), surface stellar density (Σ⋆, middle column), and volume density (ρ, right column) at selected times (in Myr). The start of each simulation is depicted as a black line and the gravitational-wave kick is always represented with a cyan line.
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: The abundances of various molecules in the HD 100453 disk compared to a selection of Class 0, I, and II objects, as well as the solar system comet 67P/C-G. Left: the abundances of CH3OCH3 and CH3OCHO relative to CH3OH, where arrows denote upper and lower limits. Here the Class II disks, aside from HD 100453, are translucent to indicate the uncertainty in the underlying CH3OH column density. Right: the isotopic ratio of 12C/13C for COMs (all CH3OH aside from IRAS 16293−2422 B, which is glycolaldehyde) and percentage D/H values for CH3OH. The filled circles show the results from this work, and the open circles are values taken from the literature. For both panels, the data for the other sources are taken from J. K. Jørgensen et al. (2016, 2018), M. Rubin et al. (2019), K. Altwegg et al. (2020), M. N. Drozdovskaya et al. (2021), Y. Yamato et al. (2024a), A. S. Booth et al. (2024a, 2024b), and J.-H. Jeong et al. (2025).
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: CH3OH emission-line spectra extracted from a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5-radius circular aperture centered on source (gray) and from a Keplerian mask with the same radial extent (purple/black). The black and gray font colors for the upper energy levels and Einstein coefficients match those in Figure 5, where only the black points are used in the rotation diagram analysis. The dashed line marks the 3σ level for the spectra from the circular aperture. This is an overestimate of the errors in the masked spectra but provides a good gauge of the significance of the detections. The final panel shows normalized 12CO J = 3–2 disk-integrated spectra for comparison, where the data are first presented in G. P. Rosotti et al. (2020).
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Moment maps of the stacked CH3OH lines imaged at different robust parameters [+2.0, +0.5, −0.5, −2.0]. From left to right the maps are the Keplerian-masked integrated intensity (M0), peak intensity (M8), and peak velocity (M9) maps. In the center map the color bar starts at the 3σ level, and the right maps have had a 5σ clip applied to the channel maps. The ellipses in the middle panel of the bottom row highlight the ringed area used to calculate the column densities.
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Disk-averaged rotation diagrams for CH3OH, 13CH3OH, and ﹩{{\rm{CH}}}_{3}{\rm{CN}}﹩ in the HD 100453 disk. The gray points in the CH3OH plot show optically thicker transitions that are excluded from the linear fit. The dashed black lines show the best-fit model, and the colors show random draws from the corresponding posterior probability distributions.
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Integrated intensity maps of the 0.9 mm dust continuum emission (taken from G. P. Rosotti et al. 2020) and molecular line emission from the HD 100453 disk. For the line maps, the text in the upper right corner notes the upper energy level of the transition shown (see Table 1), and in all plots the beam is shown in the lower left corner of each panel. The units of the color bar are mJy beam−1 km s−1 for the molecular lines and mJy beam−1 for the continuum, and the position of HD 100453 A is marked with a star.
Paper: Ice Sublimation in the Dynamic HD 100453 Disk Reveals a Rich Reservoir of Inherited Complex Organics
Authors: Alice S. Booth, Lisa Wölfer, Milou Temmink, Jenny Calahan, Lucy Evans, Charles J. Law, Margot Leemker, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Same as Figure 2, but for the other molecular lines in the data.
Paper: Candidate Dark Galaxy-2: Validation and Analysis of an Almost Dark Galaxy in the Perseus Cluster
Authors: Dayi (David) Li, 大一 李, Qing Liu, 青 刘, Gwendolyn M. Eadie, Roberto G. Abraham, Francine R. Marleau, William E. Harris, Pieter van Dokkum, Aaron J. Romanowsky, Shany Danieli, Patrick E. Brown, Alex Stringer
Figure caption: (a) Cutout images of CDG-2 obtained from binning IE-band (VIS imager) data from Euclid (left); stacked and smoothed F814W images from V12-ACS and V14-ACS images from the PIPER HST survey (middle); VIS, Y-band, and H-band combined color image from Euclid (right). Blue circles indicate the four GCs in CDG-2 while the orange dashed circle roughly outlines the region occupied by the diffuse emission in CDG-2. The diffuse emission in CDG-2 is clearly present in both data sets with similar morphology. (b) Left: Euclid IE-band data used for modeling and analyzing CDG-2. The image scale is displayed in arcsinh stretch using [0.25, 0.95] quantiles of the image. Middle left: the combined model of GCs and diffuse emission. A simulated noise level matching the data is added. Middle right: residual of the image with the combined model subtracted. Right: radial profiles of the GC + isophote model (blue) and the data (green). The orange dashed line indicates the range of isophote fitting. In the left three panels, CDG-2 is marked with a orange circle and GCs are marked with white circles.