adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Line width residuals from 12CO (3–2) predictions of inclined disks unstable to VSI, MRI, and GI. The residuals are extracted by computing the disks’ line width maps using the percentiles method in EDDY and then subtracting their azimuthal averages using GOFISH. The models only consider the upper (or front) CO layer. The images have a 104 m s−1 velocity resolution and a 35 mas angular resolution and include the noise level achieved by exoALMA. From left to right, different disk inclinations are shown. The beam size is shown in the lower left corner of each panel. The color bar limits have been adjusted for each instability.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Temperature residuals from 12CO (3–2) predictions of inclined disks unstable to VSI, MRI, and GI. The residuals are extracted by computing the disks’ eighth moment maps and then subtracting their azimuthal averages using GOFISH. The models only consider the upper (or front) CO layer. The images have a 104 m s−1 velocity resolution and a 35 mas angular resolution and include the noise level achieved by exoALMA. From left to right, different disk inclinations are shown. The beam size is shown in the lower left corner of each panel.
Paper: exoALMA. XVI. Predicting Signatures of Large-scale Turbulence in Protoplanetary Disks
Authors: Marcelo Barraza-Alfaro, Mario Flock, William Béthune, Richard Teague, Jaehan Bae, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Eric W. Koch, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gas temperature and azimuthally averaged number density of 12CO of our disk radiative transfer models. Overlaid in blue, a solid line traces the height at which the optical depth reaches unity assuming a face-on disk. The red dashed–dotted line shows the initial guess for the 12CO (3–2) emission surface in our EDDY models. The solid black line indicates the simulations’ domain in colatitude, while the gray dashed lines show spacings along Z equal to the disks’ pressure scale height.
Paper: Direct Evidence for r-process Nucleosynthesis in Delayed MeV Emission from the SGR 1806–20 Magnetar Giant Flare
Authors: Anirudh Patel, Brian D. Metzger, Jakub Cehula, Eric Burns, Jared A. Goldberg, Todd A. Thompson
Figure caption: Top panel: mass fraction of synthesized nuclei as a function of atomic mass A from our fiducial model that reproduces the late-time gamma-ray emission light curve from SGR 1806–20 (Figure 2). Vertical blue bars (right axis) show the individual percentage contributions of radioactive nuclei to the total gamma-ray energy in the time interval t = 103–104 s. Bottom panel: synthetic gamma-ray spectra from the fiducial model at three snapshots, t = 1000, 3000, 12,000 s, accounting for Doppler broadening due to the ejecta expansion but excluding extinction effects. For the spectrum at t = 3000 s, we also show with lighter blue lines the intrinsic (i.e., nonbroadened) decay lines, which contribute to the total spectrum. A thick dark gray line shows the bremsstrahlung spectral fit made by S. E. Boggs et al. (2007) in the energy range  ≈ 0.1–2.5 MeV, while a dotted light gray line shows the same fit outside of the measured energy range. The gray shaded area indicates the ±0.7 MeV uncertainty in the fit.
Paper: Direct Evidence for r-process Nucleosynthesis in Delayed MeV Emission from the SGR 1806–20 Magnetar Giant Flare
Authors: Anirudh Patel, Brian D. Metzger, Jakub Cehula, Eric Burns, Jared A. Goldberg, Todd A. Thompson
Figure caption: Parameter study exploring the isolated affects of four key parameters: Ye (top left), ﹩\bar{v}﹩ (top right), β (bottom left), and Mej (bottom right). The fiducial model is shown for comparison with a solid black line (﹩{M}_{{\rm{ej}}}\approx 1.2\times 1{0}^{-6},\,{Y}_{e}=0.40,\,\bar{v}=0.15,\,\beta =6﹩). For each model, the parameter labeled in the legend is the only one that is changed; all other parameters are held fixed at their fiducial value.
Paper: Direct Evidence for r-process Nucleosynthesis in Delayed MeV Emission from the SGR 1806–20 Magnetar Giant Flare
Authors: Anirudh Patel, Brian D. Metzger, Jakub Cehula, Eric Burns, Jared A. Goldberg, Todd A. Thompson
Figure caption: The fraction ϵγ of β-decay energy emitted as gamma rays for the fiducial model over the time range of interest (Figure 2).
Paper: Direct Evidence for r-process Nucleosynthesis in Delayed MeV Emission from the SGR 1806–20 Magnetar Giant Flare
Authors: Anirudh Patel, Brian D. Metzger, Jakub Cehula, Eric Burns, Jared A. Goldberg, Todd A. Thompson
Figure caption: GOES X-ray data (3–25 keV) around the giant-flare time. The solar X-ray flux is classified at background activity levels during the time of the delayed MeV emission; there is no solar activity that could explain the putative r-process signal.
Paper: Direct Evidence for r-process Nucleosynthesis in Delayed MeV Emission from the SGR 1806–20 Magnetar Giant Flare
Authors: Anirudh Patel, Brian D. Metzger, Jakub Cehula, Eric Burns, Jared A. Goldberg, Todd A. Thompson
Figure caption: SPI-ACS decay fit from 675 s (peak) to 12,000 s.
Paper: Unveiling a Young Thick Disk in the Milky Way
Authors: Jianhui Lian, Min Du, Shuai Lu, Bingqiu Chen, Gail Zasowski, Zhaoyu Li, Xiaojie Liao, Chao Liu
Figure caption: Vertical structure of the MAP and integrated population of the Milky Way. Left: scale height as a function of radius for various disk components. The gray dashed–dotted and black dashed lines indicate the scale height radial profiles of integrated high- and low-α populations, marked by the black and pink boxes in Figure 1, respectively. The colorful lines represent the radial profiles of low-α populations, split into mono-abundance space in [Mg/Fe] and [Fe/H], color coded by [Fe/H]. Note that the vertical axis spans only ∼7% of the distance range of the horizontal axis. Right: flaring strength (﹩{{\rm{A}}}_{{\rm{flare}}}﹩) vs. scale height at solar Galactocentric radius for high- and low-α populations. The flaring strength is represented by the best-fit slope of the scale height radial profile. The MP low-α population emphasized in the main Letter is marked with a thickened line in the left-hand panel and an enlarged circle on the right. Shaded regions and error bars represent 1σ uncertainties of the estimates of flaring strength and scale height.
Paper: Unveiling a Young Thick Disk in the Milky Way
Authors: Jianhui Lian, Min Du, Shuai Lu, Bingqiu Chen, Gail Zasowski, Zhaoyu Li, Xiaojie Liao, Chao Liu
Figure caption: Averaged age map of APOGEE stars in the [Mg/Fe]–[Fe/H] diagram across the Galaxy. [Mg/Fe]–[Fe/H] distributions are examined within the ranges of −0.9 < [Fe/H] < 0.6 and −0.15 < [Mg/Fe] < 0.5, as a function of radius (0 < R < 14 kpc in horizontal direction) and height (∣Z∣ < 4 kpc in vertical direction). Dashed contours outline the density distribution at levels of 20%, 50%, and 90% of the peak density in each panel. Pink and black boxes in the sixth column highlight the low- and high-α MAPs for which the scale height is presented in Figure 2.
Paper: Unveiling a Young Thick Disk in the Milky Way
Authors: Jianhui Lian, Min Du, Shuai Lu, Bingqiu Chen, Gail Zasowski, Zhaoyu Li, Xiaojie Liao, Chao Liu
Figure caption: Scale height and vertical velocity dispersion as a function of stellar age for mono-abundance populations (MAPs). MAPs along the old and young age–metallicity sequences are indicated as squares and circles, respectively. The separation of these two sequences is defined by a straight line in the age–metallicity plane. Color coding reflects the metallicity of each MAP. The scale height is calculated from the intrinsic density distribution of MAPs after correcting for the selection function, whereas the velocity dispersion is derived from the raw sample data. Dashed curve in the right panel represents the power law with a slope of 0.5, illustrating the predictions of the secular heating scenario (M. Martig et al. 2014).
Paper: Unveiling a Young Thick Disk in the Milky Way
Authors: Jianhui Lian, Min Du, Shuai Lu, Bingqiu Chen, Gail Zasowski, Zhaoyu Li, Xiaojie Liao, Chao Liu
Figure caption: Distribution of vertical velocity dispersion in age-[Fe/H] plane at three radii. A raw APOGEE sample is used to calculate the velocity dispersion. Gray contours in each panel outline the density distribution with levels of 30%, 60%, and 90% of the peak density. Black arrows in the left and right panels indicate the trend of decreasing vertical velocity dispersion along the two age–metallicity sequences that predominate in the inner and outer Galaxy, respectively. The orange dashed line is used to separate the two age–metallicity sequences.
Paper: Unveiling a Young Thick Disk in the Milky Way
Authors: Jianhui Lian, Min Du, Shuai Lu, Bingqiu Chen, Gail Zasowski, Zhaoyu Li, Xiaojie Liao, Chao Liu
Figure caption: Vertical velocity dispersion and maximum orbit height of integrated high- and low-α and mono-abundance low-α populations. Raw sample from the APOGEE survey is used here without correcting for the selection function. Note that the vertical axis spans only 20% of the distance range of the horizontal axis.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 4 but in the wavelength range 14–16 μm. The bottom panel shows synthetic spectra of molecules detected in this wavelength range, each normalized to their peaks. The sum of these spectra is shown in the fourth panel (red).
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: The peak-to-continuum ratio of C2H2, CO2, and H2O in the MINDS sample (and Sz114; C. Xie et al. 2023). The VLMS sources are indicated by filled circles and the T Tauri sources by empty circles. The inverted triangles indicate upper limits (tentative or nondetections). The colors are the same as in Figure 7. The dashed lines and shaded regions show the linear fits to the peak-to-continuum ratios of the different species and the 1σ standard deviation. The legend shows the correlation coefficients and p-values. The water peak corresponds to the 17.36 μm pure rotational line transition: 112,9–101,10, Eup = 2432 K. References for the spectra of T Tauri sources: S. L. Grant et al. (2023), K. R. Schwarz et al. (2024), M. Temmink et al. (2024b), B. Tabone et al. (2025, in preparation), M. Vlasblom et al. (2025).
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Overview of the stellar photospheric absorption features of water observed in the sample. The continuum-subtracted spectra are shown in black, and the water absorption models are shown in blue. The stellar photospheric absorption features in the spectra of IC 147, Sz28, and J0438 have been reported in A. M. Arabhavi et al. (2024), J. Kanwar et al. (2024a), and G. Perotti et al. (2025) respectively.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Detections of CO emission in J1605 and J1558. The continuum-subtracted spectra are shown in black, and the CO slab model is shown in orange. The J1605 spectrum is offset by 8 mJy for clarity. The slab models are arbitrarily chosen for a visual demonstration of the detections. The vertical dotted lines and the corresponding text indicate the rovibrational line transition and the spectral location. The detection of CO in J1605 has been previously reported by B. Tabone et al. (2023) and J. Kanwar et al. (2025).
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Comparison of C2H2, CO2, and H2O flux levels for the different column densities (temperatures are fixed to 325 K), normalized to the peak water flux in the shown wavelength range. Note the different vertical axis limits.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Cross-correlations of J1558 spectra with OH slab models in the wavelength regions shown in Figure 13 for different column densities (N) and temperatures (T). The correlation coefficient varies from −1 (anticorrelation, in red) to +1 (correlation, in blue). The contours of correlation coefficients at 0 and 0.75 are shown with dark gray lines. The parameter space where the statistical significance is low (i.e., the p-value is larger than 0.03) is hatched. The yellow cross indicates the best correlation coefficient.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Same as Figure 10, but stellar photospheric absorption of CO is shown in orange.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Detection of OH lines in J1558. The OH slab model is shown in green (1017 cm−2, 800 K) and the continuum-subtracted spectra in black. The water slab model is also shown in each panel (blue).
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Sketch illustrating the different components of hydrocarbon and water emission.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Flux ratios of the peaks of H2O in the 16–18 μm wavelength window and C2H2 in the 13–14 μm wavelength window. The top panels (A) show the peak flux ratios assuming the same emitting area for both molecules, and the bottom panels (B) assume a water-emitting area 4 times that of C2H2. Panels 1(A) and 1(B) assume the same column densities and temperatures for both molecules, panels 2(A) and 2(B) assume water column densities 2 orders of magnitude larger than C2H2, and panels 3(A) and 3(B) assume water model temperatures higher than the C2H2 by 200 K. The white contours correspond to flux ratios of 0.3 (solid), 0.5 (dotted), and 1 (dashed).
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Detections and nondetections of pure rotational line emission of water. The continuum-subtracted spectra are shown in black and the water slab models in blue. The slab model parameters are arbitrarily chosen for a visual match with the observed spectra. The temperature and column densities of the models are the same across all the panels, while the emitting area is scaled to match the flux level. The vertical gray area in each panel shows the wavelength region used to calculate the noise level. The light gray shaded region across the spectra shows the ±3σ noise level obtained in this way. The identified water line transitions are indicated at the top of the figure as ﹩{J}_{{K}_{a}\,{K}_{c}}-{J}_{{K}_{a}^{{\prime} }\,{K}_{c}^{{\prime} }}^{{\prime} }﹩, where J, Ka, and Kc are the total angular momentum quantum number and the projections of the angular momentum on the principal axes.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Cross-correlations of observed VLMS spectra with water slab models between 16.65 and 17.65 μm for different column densities (N) and temperatures (T). The correlation coefficient varies from −1 (anticorrelation, in red) to +1 (correlation, in blue). The contours of the correlation coefficients at 0.25, 0.5, and 0.75 are shown with dark gray lines. The parameter space where the statistical significance is low (i.e., the p-value is larger than 0.03) is hatched. The orange plus sign indicates the best correlation coefficient for each source.
Paper: MINDS: The Very Low-mass Star and Brown Dwarf Sample Hidden Water in Carbon-dominated Protoplanetary Disks
Authors: Aditya M. Arabhavi, Inga Kamp, Ewine F. van Dishoeck, Thomas Henning, Hyerin Jang, Valentin Christiaens, Danny Gasman, Ilaria Pascucci, Giulia Perotti, Sierra L. Grant, David Barrado, Manuel Güdel, Pierre-Olivier Lagage, Alessio Caratti o Garatti, Fred Lahuis, L. B. F. M. Waters, Till Kaeufer, Jayatee Kanwar, Maria Morales-Calderón, Kamber Schwarz, Andrew D. Sellek, Benoît Tabone, Milou Temmink, Marissa Vlasblom
Figure caption: Summary of the detections of emission of oxygen-bearing molecules from the inner disks of the MINDS VLMS sample. The colored boxes indicate the detections (green), nondetections (gray), and tentative detections (yellow) of oxygen-bearing species in the sample. H2Orv and H2Oro correspond to the rovibrational band and pure rotational line emission of water, respectively. The luminosities (not scaled to 150 pc) and stellar masses are obtained from C. F. Manara et al. (2023), updated based on the new Gaia EDR3 distances (Gaia Collaboration et al. 2021), except for NC1, TWA 27, and J1605, for which the missing data are taken from K. L. Luhman (2007), E. Manjavacas et al. (2024), and L. Testi et al. (2022), respectively. 2MASS source names are abbreviated above: J04381486+2611399, J04390163+2336029, J11071668–7735532, J11071860–7732516, J11074245–7733593, J11082650–7715550, J11085090–7625135, J12073346–3932539, J15582981–2310077, and J16053215–1933159.