adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: The full-sky projection of the magnetic field directions measured by Voyager 1 since 2012 August. The color coding indicates the radial distance from the Sun in astronomical units, and each point represents the magnetic field direction, calculated using hourly average data and given in longitude and latitude in RTN coordinates.
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: The trace PSD of the magnetic field fluctuations (top panel) and the normalized fluctuation amplitude δB/B0 (bottom panel) measured by Voyager 1 from 2004 to 2024. The grayed regions in top panel represent the COI in the wavelet analysis.
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: Flatnesses of the BR (blue), BT (green), and BN (red) components across the two pressure fronts in the VLISM using 48 s cadence data. The upstream period of pf1 spans 2016 June 1 to 2016 December 1, and the downstream period spans 2016 December 20 to 2017 June 1. For pf2, the upstream period is from 2020 January 1 to 2020 May 20, and the downstream period is from 2020 June 1 to 2020 December 31.
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: The evolution of magnetic compressibility following Voyager 1’s TS crossing. Magnetic compressibility is defined as the ratio of the magnetic magnitude fluctuation power to the total trace power, ﹩{C}_{B}={P}_{| B| }/{P}_{{\rm{Tr}}}﹩. The grayed regions represent the COI in the wavelet analysis.
Paper: Electromagnetic Energy Extraction from Kerr Black Holes: Ab Initio Calculations
Authors: Claudio Meringolo, Filippo Camilloni, Luciano Rezzolla
Figure caption: Spacetime diagrams of the total number density along the equatorial plane for BHs with spin a* = 0.7 (left panel), a* = 0.9 (middle panel), and a* = 0.999 (right panel). The insets offer magnifications close to the event horizon and the vertical dashed lines mark the location of the ergosphere r0. The peaks of the number density track the motions of the plasmoids, which can collide (red square) and split (red circles) within the ergosphere; outgoing plasmoids are accelerated at relativistic speeds vr ∼ 0.7 (see the slope).
Paper: Electromagnetic Energy Extraction from Kerr Black Holes: Ab Initio Calculations
Authors: Claudio Meringolo, Filippo Camilloni, Luciano Rezzolla
Figure caption: Left panel: total number density of particles normalized to the Goldreich–Julian density n/nGJ as measured by a FIDO observer. The data refer to time ﹩\bar{t}=10\,M﹩ and to a BH with spin a* = 0.999. Also shown are the ergosphere (cyan dashed line), the inner and outer light surfaces (blue solid lines), and the stagnation surface (red solid line). Right panel: the same as the left for but for the Lorentz factor Γ.
Paper: Electromagnetic Energy Extraction from Kerr Black Holes: Ab Initio Calculations
Authors: Claudio Meringolo, Filippo Camilloni, Luciano Rezzolla
Figure caption: BZ luminosity PBZ normalized to the maximum value of the lowest-order (i.e., quadratic) expression ﹩{P}_{{\rm{BZ0}}}^{{}_{{\rm{\max }}}}﹩, as a function of the BH angular velocity (see the top horizontal axis for a mapping in terms of the BH dimensionless spin) for all of our GRPIC simulations (black filled circles) and with the associated numerical errors. The black solid line shows the analytic expression (Equation (5)) after rescaling the factor κ to account for the specific magnetic field topology (one-parameter fit). Also reported are the data from GRMHD simulations (A. Tchekhovskoy et al. 2010; red filled circles) and the corresponding analytic expression suitably rescaled for κ (red solid line). Shown in the inset with dashed lines of corresponding colors are the fits to the data in terms of the coefficients κ and ﹩\tilde{\beta }﹩ (two-parameter fit).
Paper: Electromagnetic Energy Extraction from Kerr Black Holes: Ab Initio Calculations
Authors: Claudio Meringolo, Filippo Camilloni, Luciano Rezzolla
Figure caption: Spacetime diagrams for the average energy at infinity of positrons 〈e+,∞〉 (top row) and electrons 〈e−,∞〉 (bottom row) for the same simulations reported in Figure 2. Note how negative-energy positrons are present even at moderate spins and their abundances and energies increase with the BH spin. In the case of electrons, only the highest spin leads to the generation of negative-energy electrons. As in Figure 2, the squares and circles are used to highlight the collision or splitting of plasmoids within the ergosphere.
Paper: Electromagnetic Energy Extraction from Kerr Black Holes: Ab Initio Calculations
Authors: Claudio Meringolo, Filippo Camilloni, Luciano Rezzolla
Figure caption: Averaged reconnection rate ﹩{ \mathcal R }﹩ reported as a function of the spin a* and the distance from the horizon ﹩{ \mathcal D }﹩. The average is computed in the time window ﹩0\,\leqslant \,\bar{t}/M\,\leqslant \,40﹩ and with a spatial resolution of 0.5 M. The cyan dashed line shows the position of the ergosphere r0 for different BH spins.
Paper: The Rings of (2060) Chiron: Evidence of an Evolving System
Authors: C. L. Pereira, F. Braga-Ribas, B. Sicardy, R. Leiva, M. Assafin, B. E. Morgado, J. L. Ortiz, P. Santos-Sanz, J. I. B. Camargo, G. Margoti, Y. Kilic, G. Benedetti-Rossi, R. Vieira-Martins, T. F. L. L. Pinheiro, R. Sfair, F. L. Rommel, A. R. Gomes-Júnior, R. C. Boufleur, R. Duffard, J. Desmars, D. Souami, N. Morales, F. Arrese, K. Barkaoui, A. Burdanov, C. A. Colazo, C. A. Domingues, H. Dutra, R. C. Gargalhone, C. Jacques, F. Jablonski, L. Liberato, R. Melia, J. C. Oliveira, M. Sardiña, J. Spagnotto, T. Speranza, A. Wilberger, M. A. Zorzan, L. S. Brito, J. P. Cavalcante, T. Q. Costa, M. Emilio, E. Garcia-Migani, M. Gillon, E. Gradovski, E. Jehin, V. Lattari, M. Malacarne, L. A. Mammana, M. Melita, W. Melo, A. J. Ortiz, P. Quitral-Manosalva, G. Ramon, I. Rodrigues, L. Vanzi
Figure caption: Left: sky-plane projection of the shell model. The color map shows the optical depth ﹩\tau =-{\mathrm{ln}}\,(T)/2﹩ from three Gaussian-distributed spherical shells. The central gray circle (98 km radius) marks Chiron’s projected size; black ellipses indicate the confined rings; and red circles denote the Roche limits. Right: sky-plane view of the equatorial disk model. Optical depth ﹩\tau ={\tau }_{{\rm{N}}}/| \sin (B)| ﹩ is shown. The gray circle (98 km radius) marks Chiron. Black ellipses show the three narrow rings; dashed blue ellipses mark the 1/2 and 1/3 SORs; and red ellipses indicate Roche limits. Inset: zoom-in of the innermost region with rings Chi1R (1), Chi2R (2), and Chi3R (3).
Paper: The Rings of (2060) Chiron: Evidence of an Evolving System
Authors: C. L. Pereira, F. Braga-Ribas, B. Sicardy, R. Leiva, M. Assafin, B. E. Morgado, J. L. Ortiz, P. Santos-Sanz, J. I. B. Camargo, G. Margoti, Y. Kilic, G. Benedetti-Rossi, R. Vieira-Martins, T. F. L. L. Pinheiro, R. Sfair, F. L. Rommel, A. R. Gomes-Júnior, R. C. Boufleur, R. Duffard, J. Desmars, D. Souami, N. Morales, F. Arrese, K. Barkaoui, A. Burdanov, C. A. Colazo, C. A. Domingues, H. Dutra, R. C. Gargalhone, C. Jacques, F. Jablonski, L. Liberato, R. Melia, J. C. Oliveira, M. Sardiña, J. Spagnotto, T. Speranza, A. Wilberger, M. A. Zorzan, L. S. Brito, J. P. Cavalcante, T. Q. Costa, M. Emilio, E. Garcia-Migani, M. Gillon, E. Gradovski, E. Jehin, V. Lattari, M. Malacarne, L. A. Mammana, M. Melita, W. Melo, A. J. Ortiz, P. Quitral-Manosalva, G. Ramon, I. Rodrigues, L. Vanzi
Figure caption: Occultation profile from the PE160 observation on 2023 September 10 event of the normal optical depth as a function of radial distance in the ring plane shows the extent of the broad ring and the arrangement of the dense rings. The colored regions indicate the boundaries of the SOR 1/2 resonance (green), SOR 1/3 resonance (red), and the Roche limit (blue). The vertical dotted lines indicate the respective ring center.
Paper: The Rings of (2060) Chiron: Evidence of an Evolving System
Authors: C. L. Pereira, F. Braga-Ribas, B. Sicardy, R. Leiva, M. Assafin, B. E. Morgado, J. L. Ortiz, P. Santos-Sanz, J. I. B. Camargo, G. Margoti, Y. Kilic, G. Benedetti-Rossi, R. Vieira-Martins, T. F. L. L. Pinheiro, R. Sfair, F. L. Rommel, A. R. Gomes-Júnior, R. C. Boufleur, R. Duffard, J. Desmars, D. Souami, N. Morales, F. Arrese, K. Barkaoui, A. Burdanov, C. A. Colazo, C. A. Domingues, H. Dutra, R. C. Gargalhone, C. Jacques, F. Jablonski, L. Liberato, R. Melia, J. C. Oliveira, M. Sardiña, J. Spagnotto, T. Speranza, A. Wilberger, M. A. Zorzan, L. S. Brito, J. P. Cavalcante, T. Q. Costa, M. Emilio, E. Garcia-Migani, M. Gillon, E. Gradovski, E. Jehin, V. Lattari, M. Malacarne, L. A. Mammana, M. Melita, W. Melo, A. J. Ortiz, P. Quitral-Manosalva, G. Ramon, I. Rodrigues, L. Vanzi
Figure caption: Comparison between the equatorial disk and shell models. In the panels, the black curve represents the corresponding model compared to the observed light curve. (a) The time-based light curve is projected in the radial distance on the ring plane considering the preferred mean pole orientation. (b) The normalized flux as a function as the radial distance in the sky plane, compared with the model based in the consecutive spherical shells. The residuals plus 1 for the equatorial disk (c) and shell (d) models.
Paper: The Rings of (2060) Chiron: Evidence of an Evolving System
Authors: C. L. Pereira, F. Braga-Ribas, B. Sicardy, R. Leiva, M. Assafin, B. E. Morgado, J. L. Ortiz, P. Santos-Sanz, J. I. B. Camargo, G. Margoti, Y. Kilic, G. Benedetti-Rossi, R. Vieira-Martins, T. F. L. L. Pinheiro, R. Sfair, F. L. Rommel, A. R. Gomes-Júnior, R. C. Boufleur, R. Duffard, J. Desmars, D. Souami, N. Morales, F. Arrese, K. Barkaoui, A. Burdanov, C. A. Colazo, C. A. Domingues, H. Dutra, R. C. Gargalhone, C. Jacques, F. Jablonski, L. Liberato, R. Melia, J. C. Oliveira, M. Sardiña, J. Spagnotto, T. Speranza, A. Wilberger, M. A. Zorzan, L. S. Brito, J. P. Cavalcante, T. Q. Costa, M. Emilio, E. Garcia-Migani, M. Gillon, E. Gradovski, E. Jehin, V. Lattari, M. Malacarne, L. A. Mammana, M. Melita, W. Melo, A. J. Ortiz, P. Quitral-Manosalva, G. Ramon, I. Rodrigues, L. Vanzi
Figure caption: Sky-plane projection of Chiron and its confined rings. The projected ellipsoid and the occulting chords for each event are plotted in turquoise, with their 1σ uncertainties represented by the red segments at the chord extremities. The dashed blue lines represent the occulting chords as seen from each site. The red segments mark the projected widths of the ring events plus their respective 1σ error bars. The labels 1, 2, and 3 refers to the Chi1R, Chi2R, and Chi3R rings, respectively.
Paper: Resolving Black Hole Family Issues among the Massive Ancestors of Very High-spin Gravitational-wave Events like GW231123
Authors: Jakob Stegmann, Aleksandra Olejak, Selma E. de Mink
Figure caption: Cartoons of formation scenarios considered in this work. For purely dynamical scenarios, we assume that the primary black hole is formed through a hierarchical sequence 1g+1g (red), 2g+2g (blue), 2g+1g (turquoise), and 3g+1g (orange), and subsequently merges with a secondary black hole in a GW231123-like event. For these dynamical formation sequences, we assume the first-generation black holes (1g) to be slowly spinning (R. Abbott et al. 2023) the remnants to obtain a large spin. At each merger, the directions of the spin and orbital angular momentum vectors are fully randomized. Alternatively, we consider a scenario where the primary black hole forms from massive binary star evolution (green), e.g., of primordial stellar binaries in a star cluster, before it dynamically assembles and merges with the secondary black hole. Here, we assume the 1g black holes to obtain aligned spins (exploring different assumptions about their magnitudes) through binary star evolution, which leads to much higher primary spins χf ≈ 0.9.
Paper: Resolving Black Hole Family Issues among the Massive Ancestors of Very High-spin Gravitational-wave Events like GW231123
Authors: Jakob Stegmann, Aleksandra Olejak, Selma E. de Mink
Figure caption: Recoil kick velocity distribution (left panel) and remnant spin distribution (right panel) of black holes formed through 1g+1g (red), 2g+1g (turquoise), 2g+2g (blue), and 3g+1g (orange) merger sequences. For all mergers, it is assumed that the black hole spin and orbital angular momentum directions are randomly distributed. For the colored solid lines, we assume all mergers result from incoming black holes of the same mass. The dashed turquoise and orange lines assume q = 1/2 and q = 1/3 for 2g+1g and 3g+1g, respectively. The vertical dashed line in the left panel indicates the adopted ejection velocity vej = 100 km s−1, beyond which remnant black holes are removed from participating in further mergers (see the main text). In the right panel, we show GW231123’s Combined posterior distributions for the primary (black) and secondary spin (gray) from the public LVK data release (The LIGO Scientific Collaboration et al. 2025d). Vertical dashed and dotted lines indicate their 0.1, 0.5, and 0.9 quantiles, respectively.
Paper: Resolving Black Hole Family Issues among the Massive Ancestors of Very High-spin Gravitational-wave Events like GW231123
Authors: Jakob Stegmann, Aleksandra Olejak, Selma E. de Mink
Figure caption: Posterior samples of 13 massive binary black hole merger events (median Mf > 100 M⊙ and Mf consistent with ﹩{m}_{1}=13{7}_{-17}^{+22}\,{M}_{\odot }﹩) contained in the cumulative Gravitational-Wave Transient Catalog 4.0 (The LIGO Scientific Collaboration et al. 2025b). The posterior samples are retrieved from public data releases (The LIGO Scientific Collaboration & the Virgo Collaboration 2022, 2023; The LIGO Scientific Collaboration et al. 2025c). Thick purple lines indicate the posteriors of GW231028, which is the only event with strong support for nonzero χeff, while error bars indicate the primary mass and spin uncertainties of GW231123, respectively.
Paper: Resolving Black Hole Family Issues among the Massive Ancestors of Very High-spin Gravitational-wave Events like GW231123
Authors: Jakob Stegmann, Aleksandra Olejak, Selma E. de Mink
Figure caption: Same as Figure 2 for our primordial binary star scenario, where the ancestral black holes of GW231123 are assumed to have equal masses and spins aligned with the orbital angular momentum. For the green line, we assume both black holes to be slowly spinning, for the purple line, we assume just one to be highly spinning, and for the gold line, we assume both to be highly spinning (see the main text for details).
Paper: Insights for Early Massive Black Hole Growth from JWST Detection of the [Ne v] λ3427 Emission Line
Authors: Benny Trakhtenbrot, Claudio Ricci, Ezequiel Treister, Michael J. Koss, Richard Mushotzky, Kyuseok Oh, Alessandro Peca, Franz E. Bauer, Kriti Kamal Gupta, Tomer Reiss
Figure caption: The SMBH–host mass plane with the ﹩\left[{\rm{Ne}}\,{\rm\small{V}}\right]﹩-based constraints for the two z > 5 AGN studied here. We plot the two lower limits on BH masses, ﹩{M}_{{\rm{BH}},{\rm{\min }}}﹩ (colored triangles), derived by scaling the ﹩\left[{\rm{Ne}}\,{\rm\small{V}}\right]﹩ line emission to Lbol (via Equation (1)) and assuming Lbol ≤ LEdd. The systematic uncertainties associated with this scaling (0.6 dex), and with the assumption of Lbol = LEdd (see text), are illustrated by the large pink marker (bottom-right corner). For GN 42437, we also plot an alternative estimate (lower open triangle), assuming that only one-third of the ionizing radiation is due to an AGN, as suggested by C24 (a highly conservative assumption for ﹩\left[{\rm{Ne}}\,{\rm\small{V}}\right]﹩; see text). We include for comparison several other samples from the local and distant (z > 5) Universe (see legend): local ellipticals (from J. Kormendy & L. C. Ho 2013; large gray circles), low-z broad-line AGN (from A. E. Reines & M. Volonteri 2015; small gray circles); luminous z ≳ 6 quasars selected from ground-based, wide-field optical–near-infrared surveys (from M. Yue et al. 2024b and X. Ding et al. 2023; filled blue symbols); and several fainter, broad-line AGN identified in various spectroscopic JWST studies (from Y. Harikane et al. 2023; H. Übler et al. 2023; R. Maiolino et al. 2024; and J. E. Greene et al. 2024; open blue symbols). Diagonal dotted lines denote BH-to-stellar mass ratios of MBH/M* = 1: 1000, 100, 10, and 1. The two sources studied here appear to have extremely high mass ratios, MBH/M* ≈ 0.1–1.
Paper: Insights for Early Massive Black Hole Growth from JWST Detection of the [Ne v] λ3427 Emission Line
Authors: Benny Trakhtenbrot, Claudio Ricci, Ezequiel Treister, Michael J. Koss, Richard Mushotzky, Kyuseok Oh, Alessandro Peca, Franz E. Bauer, Kriti Kamal Gupta, Tomer Reiss
Figure caption: The [Ne v] λ3427/[Ne III] λ3870 vs. ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]\,\lambda 5007﹩/Hβ line ratio diagnostic diagram, with regions dominated by various ionization mechanisms marked following N. J. Cleri et al. (2023). The two galaxies under study (large colored symbols) are consistent with AGN-driven photoionization, albeit with some contribution from other sources for GN 42437. Low-redshift, bona fide narrow-line AGN (black crosses; drawn from BASS/DR2; K. Oh et al. 2022) have similar line ratios to those of the two high-redshift galaxies we study here. We argue that the high ﹩\left[{\rm{Ne}}\,{\rm\small{V}}\right]﹩ line luminosity, that is ﹩{L}_{\left[{\rm{Ne}}\,{\rm\small{V}}\right]}﹩ itself, should also be considered when interpreting the ionization mechanism.
Paper: Separating Photospheric and Starspot Magnetic Fields in Pre-main-sequence Stars Using IGRINS Spectroscopy
Authors: Facundo Pérez Paolino, Lynne A. Hillenbrand, Jeffrey S. Bary
Figure caption: Comparison of synthetic spectra for a two-field configuration to a single-field configuration for the six wavelength regions used in fitting, each with the same mean magnetic flux and projected rotational velocity ﹩v\sin i=10\,{\rm{km}}\,{{\rm{s}}}^{-1}﹩. The two-field model has Bphot = 1 kG and Bspot = 3 kG with fspot = 0.5, while the single-field model has Bphot = Bspot = 2 kG and fspot = 0.5. Both models have Tphot = 4250 K and Tspot = 3600 K. Left panels show the normalized flux in each wavelength interval; right panels show the fractional residuals between the two models. Residual amplitudes of 1%–4% occur across multiple magnetically sensitive lines, indicating that high-S/N (≳100) spectra should permit detection of such differences in real data.
Paper: Separating Photospheric and Starspot Magnetic Fields in Pre-main-sequence Stars Using IGRINS Spectroscopy
Authors: Facundo Pérez Paolino, Lynne A. Hillenbrand, Jeffrey S. Bary
Figure caption: Comparison of IGRINS spectra (blue) to the best-fitting two-component spot models (orange) for Haro 1–8 across selected wavelength regions. The total model (orange) is decomposed into the starspots (red) and the unspotted photosphere (green). A horizontal dashed line marks the normalized continuum level. Strong lines are marked throughout, with the CO bandhead region shaded in light blue.
Paper: Separating Photospheric and Starspot Magnetic Fields in Pre-main-sequence Stars Using IGRINS Spectroscopy
Authors: Facundo Pérez Paolino, Lynne A. Hillenbrand, Jeffrey S. Bary
Figure caption: Magnetic field strengths and starspot filling factors for the sample. (a) Effective temperature vs. photospheric (Bphot), spot (Bspot), and surface-averaged (Baverage) magnetic field strengths, shown as colored points with 1σ uncertainties. (b) Bphot vs. fspot. (c) Bspot vs. fspot. All panels include marginal kernel density estimates along the top and right axes to illustrate the distributions of each quantity; in panel (a), the right marginals are color-coded to match the three field strength components. The absence of clear monotonic trends in panels (b) and (c) is consistent with the low correlation coefficients reported in Section 4.
Paper: Separating Photospheric and Starspot Magnetic Fields in Pre-main-sequence Stars Using IGRINS Spectroscopy
Authors: Facundo Pérez Paolino, Lynne A. Hillenbrand, Jeffrey S. Bary
Figure caption: Posterior probability distributions for the fitted parameters of Haro 1–8 derived using the two-component spotted magnetic model. Vertical lines mark the median and ±3σ intervals. Off-diagonal panels show the corresponding two-dimensional marginalized distributions for each parameter pair, with contours enclosing the 1σ, 2σ, and 3σ confidence regions.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The left panel shows the three-color mosaic of the LMC combining Herschel/HERITAGE SPIRE 500 μm (red) and 250 μm (green) and PACS 160 μm (blue; M. Meixner et al. 2013) images with the positions of star-forming regions N158 (hosting ST6) and 30 Dor indicated. The yellow rectangle outlines the field of view of the image shown in the right panel: a three-color mosaic of N158, combining Spitzer/SAGE IRAC 8.0 μm (red), 4.5 μm (green; M. Meixner et al. 2006), and MCELS Hα (blue; R. C. Smith & MCELS Team 1998) images. The position of ST6 is indicated with a white circle and labeled. The inset shows a zoom-in on ST6 and its surroundings. The contours represent the 13CO (2–1) emission with contour levels of (10, 20, 40, 80)% of the emission peak of 12.4 Jy beam−1 km s−1; the synthesized beam size is 7″ × 7″. See Appendix A for more details.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: Ice abundances with respect to H2O ice of ST6 compared to those of Galactic protostars with large COM ice detections: the high-mass protostars IRAS 23385 (W. R. M. Rocha et al. 2024b) and IRAS 18089 (E. F. van Dishoeck et al. 2025) and low-mass protostars (hot corinos) IRAS 2A (Y. Chen et al. 2024; W. R. M. Rocha et al. 2024b) and B1–c (Y. Chen et al. 2024). The ice abundances for IRAS 2A are from W. R. M. Rocha et al. (2024b). The 13.2 μm H2O band was used to determine ﹩{N}_{{{\rm{H}}}_{2}{\rm{O}},\,\mathrm{ice}}﹩ for all the sources. The hatches and arrows indicate tentative detections and upper limits, respectively.