adsabs/AstroCLIMB huggingface dataset:
Paper: Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
Authors: Theodore Kareta, Cristina Thomas, Jian-Yang Li, Matthew M. Knight, Nicholas Moskovitz, Agata Rożek, Michele T. Bannister, Simone Ieva, Colin Snodgrass, Petr Pravec, Eileen V. Ryan, William H. Ryan, Eugene G. Fahnestock, Andrew S. Rivkin, Nancy Chabot, Alan Fitzsimmons, David Osip, Tim Lister, Gal Sarid, Masatoshi Hirabayashi, Tony Farnham, Gonzalo Tancredi, Patrick Michel, Richard Wainscoat, Rob Weryk, Bonnie Burrati, Jana Pittichová, Ryan Ridden-Harper, Nicole J. Tan, Paul Tristram, Tyler Brown, Mariangela Bonavita, Martin Burgdorf, Elahe Khalouei, Penelope Longa, Markus Rabus, Sedighe Sajadian, Uffe Graae Jorgensen, Martin Dominik, Jean-Baptiste Kikwaya, Elena Mazzotta Epifani, Elisabetta Dotto, Prasanna Deshapriya, Pedro Hasselmann, Massimo Dall'Ora, Lyu Abe, Tristan Guillot, Djamel Mékarnia, Abdelkrim Agabi, Philippe Bendjoya, Olga Suarez, Amaury Triaud, Thomas Gasparetto, Maximillian N. Günther, Michael Kueppers, Bruno Merin, Joseph Chatelain, Edward Gomez, Helen Usher, Cai Stoddard-Jones, Matthew Bartnik, Michael Bellaver, Brenna Chetan, Emma Dugan, Tori Fallon, Jeremy Fedewa, Caitlyn Gerhard, Seth A. Jacobson, Shane Painter, David-Michael Peterson, Joseph E. Rodriguez, Cody Smith, Kirill V. Sokolovsky, Hannah Sullivan, Kate Townley, Sarah Watson, Levi Webb, Josep M. Trigo-Rodríguez, Josep M. Llenas, Ignacio Pérez-García, A. J. Castro-Tirado, Jean-Baptiste Vincent, Alessandra Migliorini, Monica Lazzarin, Fiorangela La Forgia, Fabio Ferrari, Tom Polakis, Brian Skiff
Figure caption: Collection of telescopic images showcasing the evolution of the ejecta from the DART impact. The images are identically scaled and oriented (north-up, each is 100″ across) such that observations from different facilities can be compared, and a small legend in the lower left of each sub-panel shows the anti-sunward and anti-velocity vectors. The ejecta reaches a peak in perceived complexity in the first few days, but as the ejecta fans spread out, the anti-sunward tail becomes the only clearly discernible feature by approximately day T+15 to T+20. The “second” tail seen in HST observations can be discerned in data taken in good conditions (see middle panel, right, T+14.51 days, with two arrows to indicate the direction of the two tails) several days after it was first seen from space.
Paper: Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
Authors: Theodore Kareta, Cristina Thomas, Jian-Yang Li, Matthew M. Knight, Nicholas Moskovitz, Agata Rożek, Michele T. Bannister, Simone Ieva, Colin Snodgrass, Petr Pravec, Eileen V. Ryan, William H. Ryan, Eugene G. Fahnestock, Andrew S. Rivkin, Nancy Chabot, Alan Fitzsimmons, David Osip, Tim Lister, Gal Sarid, Masatoshi Hirabayashi, Tony Farnham, Gonzalo Tancredi, Patrick Michel, Richard Wainscoat, Rob Weryk, Bonnie Burrati, Jana Pittichová, Ryan Ridden-Harper, Nicole J. Tan, Paul Tristram, Tyler Brown, Mariangela Bonavita, Martin Burgdorf, Elahe Khalouei, Penelope Longa, Markus Rabus, Sedighe Sajadian, Uffe Graae Jorgensen, Martin Dominik, Jean-Baptiste Kikwaya, Elena Mazzotta Epifani, Elisabetta Dotto, Prasanna Deshapriya, Pedro Hasselmann, Massimo Dall'Ora, Lyu Abe, Tristan Guillot, Djamel Mékarnia, Abdelkrim Agabi, Philippe Bendjoya, Olga Suarez, Amaury Triaud, Thomas Gasparetto, Maximillian N. Günther, Michael Kueppers, Bruno Merin, Joseph Chatelain, Edward Gomez, Helen Usher, Cai Stoddard-Jones, Matthew Bartnik, Michael Bellaver, Brenna Chetan, Emma Dugan, Tori Fallon, Jeremy Fedewa, Caitlyn Gerhard, Seth A. Jacobson, Shane Painter, David-Michael Peterson, Joseph E. Rodriguez, Cody Smith, Kirill V. Sokolovsky, Hannah Sullivan, Kate Townley, Sarah Watson, Levi Webb, Josep M. Trigo-Rodríguez, Josep M. Llenas, Ignacio Pérez-García, A. J. Castro-Tirado, Jean-Baptiste Vincent, Alessandra Migliorini, Monica Lazzarin, Fiorangela La Forgia, Fabio Ferrari, Tom Polakis, Brian Skiff
Figure caption: Deep 327 s SDSS r composite image of the DART ejecta taken with the SOAR telescope on UTC September 29. Didymos and Dimorphos are at the center of the brightest area at left, the ejecta fans spread toward the left in the approximate opposite of the direction of DART's trajectory, and the tail can be seen stretching at least 10,000 km outwards in the anti-sunward direction. The features are described in the text and shown to develop in Figure 4, where this image becomes the top-center frame. We note explicitly that the faint structure to the south-west of the asteroids is a stacking artifact.
Paper: Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
Authors: Theodore Kareta, Cristina Thomas, Jian-Yang Li, Matthew M. Knight, Nicholas Moskovitz, Agata Rożek, Michele T. Bannister, Simone Ieva, Colin Snodgrass, Petr Pravec, Eileen V. Ryan, William H. Ryan, Eugene G. Fahnestock, Andrew S. Rivkin, Nancy Chabot, Alan Fitzsimmons, David Osip, Tim Lister, Gal Sarid, Masatoshi Hirabayashi, Tony Farnham, Gonzalo Tancredi, Patrick Michel, Richard Wainscoat, Rob Weryk, Bonnie Burrati, Jana Pittichová, Ryan Ridden-Harper, Nicole J. Tan, Paul Tristram, Tyler Brown, Mariangela Bonavita, Martin Burgdorf, Elahe Khalouei, Penelope Longa, Markus Rabus, Sedighe Sajadian, Uffe Graae Jorgensen, Martin Dominik, Jean-Baptiste Kikwaya, Elena Mazzotta Epifani, Elisabetta Dotto, Prasanna Deshapriya, Pedro Hasselmann, Massimo Dall'Ora, Lyu Abe, Tristan Guillot, Djamel Mékarnia, Abdelkrim Agabi, Philippe Bendjoya, Olga Suarez, Amaury Triaud, Thomas Gasparetto, Maximillian N. Günther, Michael Kueppers, Bruno Merin, Joseph Chatelain, Edward Gomez, Helen Usher, Cai Stoddard-Jones, Matthew Bartnik, Michael Bellaver, Brenna Chetan, Emma Dugan, Tori Fallon, Jeremy Fedewa, Caitlyn Gerhard, Seth A. Jacobson, Shane Painter, David-Michael Peterson, Joseph E. Rodriguez, Cody Smith, Kirill V. Sokolovsky, Hannah Sullivan, Kate Townley, Sarah Watson, Levi Webb, Josep M. Trigo-Rodríguez, Josep M. Llenas, Ignacio Pérez-García, A. J. Castro-Tirado, Jean-Baptiste Vincent, Alessandra Migliorini, Monica Lazzarin, Fiorangela La Forgia, Fabio Ferrari, Tom Polakis, Brian Skiff
Figure caption: Reduced magnitudes for a subset of the data shown in Figures 1 and 2 converted to cross-sectional area through the same HG1G2 model as in the Figure 1 phase function and an average albedo of p  r  = 0.15. Accounting for the pre-impact brightness of Didymos and Dimorphos, the total cross-sectional area is halved by the T+8 brightness change event.
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: Top left: representative [C I] 1–0 channels showing the upper (solid) and lower (dashed) emission surfaces with isovelocity contours of the best-fitting model overlaid. The LSRK velocity and synthesized beam are shown in the the upper right and bottom left corner, respectively, of each panel. Top right: derived [C I] 1–0 emission surface showing both radially binned (large points) and individual measurements (small points). The orange line shows the exponentially tapered power-law fit, where the solid line shows the radial range used in the fitting and the dashed line is an extrapolation. Lines of constant z/r from 0.1 to 0.6 are shown in gray. Bottom: channel maps of 12CO J = 2–1 with [C I] 1–0 emission overlaid in orange. The 12CO data are taken from Öberg et al. (2021). The synthesized beams are shown in the lower left corner of each panel.
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: [C I] 1–0 zeroth moment map (left) and 490 GHz continuum image (right) of the IM Lup disk. The synthesized beam and a scale bar indicating 100 au is shown in the lower left and right corner, respectively, of each panel.
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Estimated gas disk lifetime t life,g as a function of M *. The blue line indicates t life,g for the EUV-only case. The gray line adds X-ray photoevaporation. The spectral type corresponding to each M * is presented on the top axis. Note that these lifetimes apply only to small grain–depleted disks and not to disks where FUV photoelectric heating drives photoevaporation.
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Detection rates of gaseous debris disks are highest among young A-type stars. The tracers are CO millimeter emission (left), C II 157  μm (middle), and O I 63  μm (right). The light green histograms show the all-survey count and are superposed by dark green histograms indicating the detection count for sources younger than 50 Myr. The light and dark yellow histograms are sources older than 50 Myr. The horizontal axis gives the stellar type. Integrated counts are shown for M, K, and G stars. All data are from Hughes et al.’s (2018) Table 1. These trends are consistent with the M *-dependence of our predicted lifetimes in Figure 1.
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: Top: azimuthally averaged [C I] 1–0 radial intensity (gray) and peak intensity (blue) profiles deprojected using the derived emission surface. Shaded regions show the 1σ uncertainty. The FWHM of the major axis of the synthesized beam is shown by a horizontal bar in the upper right. Middle: optical depth profile of [C I] 1–0. Bottom: radial C I column density profile. Both optical depth and N col profiles assume thermal line widths and a constant excitation temperature of 50 K. Horizontal lines show values derived from spatially resolved ALMA observations of HD 163296 (Alarcón et al. 2022), HD 169142 (Booth et al. 2023), and HD 142527 (Temmink et al. 2023). The horizontal shaded region indicates 1/2× the beam major axis in all panels.
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: [C I] 1–0 (points) and 12CO J = 2–1 (solid line) emitting heights compared to the thermochemical model (background) tuned to the IM Lup disk from Cleeves et al. (2016) showing gas temperature (top), gas density (middle), and UV field (bottom), The UV field is the stellar-integrated flux from 930 to 2000 Å, including Lyα, plus an external radiation field (G 0 = 4) from Cleeves et al. (2016).
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Same axes as Figure 1. Solid, dashed, and dotted–dashed lines show lifetimes of slow-wind, fast-wind, and laminar disks, respectively. The dotted lines show the median lifetimes of the population synthesis in Appendix D.
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: [C I] 1–0 emission surface in the IM Lup disk vs. that of the CO isotopologues and small dust heights (left); and CN and C2H (right). The 12CO J = 2–1 and 13CO J = 2–1 heights are taken from Law et al. (2021b), the NIR scattering surface is from Avenhaus et al. (2018), and the CN N = 3–2 and C2H N = 4–3 heights are from Paneque-Carreño et al. (2023a).
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Derived t life,g with accretion-generated EUV (blue). The lifetimes of the fiducial runs are also plotted for comparison (light blue).
Paper: CI Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk
Authors: Charles J. Law, Felipe Alarcón, L. Ilsedore Cleeves, Karin I. Öberg, Teresa Paneque-Carreño
Figure caption: Channel maps of [C I] 1–0 emission in the IM Lup disk. The synthesized beam is shown in the lower left corner of each panel and the LSRK velocity in km s−1 is printed in the upper right.
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Gas lifetime (t life,g), switching time (t 0), and estimated inner gas disk lifetime (t w) for the EUV (top) and EUV+X-ray (bottom) models with slow-wind, fast-wind, and laminar disks. Thicker lines represent scenarios excluding accretion-generated EUV (Appendix C), while thinner lines depict those with it. In the bottom left and right panels, t w is omitted for M * < 3 M ⊙, except for M * = 2 M ⊙ in the bottom left panel, since t w is not found in t > 0.01 Myr. In the middle panels (fast-wind disks), the lines for t 0 and t w almost overlap.
Paper: A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars
Authors: Riouhei Nakatani, Neal J. Turner, Yasuhiro Hasegawa, Gianni Cataldi, Yuri Aikawa, Sebastián Marino, Hiroshi Kobayashi
Figure caption: Resulting population. The blue and gray histograms are the probability densities for the EUV and EUV+X-ray models, respectively. Corresponding normalized cumulative probabilities are shown by the solid lines with the same colors.
Paper: TOI-1670 c, a 40 day Orbital Period Warm Jupiter in a Compact System, Is Well Aligned
Authors: Jack Lubin, Xian-Yu Wang, Malena Rice, Jiayin Dong, Songhu Wang, Brandon T. Radzom, Paul Robertson, Gudmundur Stefansson, Jaime A. Alvarado-Montes, Corey Beard, Chad F. Bender, Arvind F. Gupta, Samuel Halverson, Shubham Kanodia, Dan Li, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: A combined fit of photometry, nontransit radial velocity data, and Rossiter–McLaughlin measurements was conducted for TOI-1670 c. Panel (a) displays the modeling of TESS  transits. The gray dots represent the phase-folded transit, while the red dashed line illustrates the modeled light curve. Panel (b) presents the radial velocity fit using RV data from various spectrographs, namely TULL, FIES, and HARPS-N. The observed data are differentiated by unique markers and colors for each instrument, and the red dashed line depicts the modeled RV curve. Panels (c) and (d) detail the RM modeling based on allesfitter and rmfit, respectively. The RM data are represented by blue dots, and the RM model is shown in red. Gray regions indicate the 1σ credible intervals. Residuals are displayed beneath each panel.
Paper: TOI-1670 c, a 40 day Orbital Period Warm Jupiter in a Compact System, Is Well Aligned
Authors: Jack Lubin, Xian-Yu Wang, Malena Rice, Jiayin Dong, Songhu Wang, Brandon T. Radzom, Paul Robertson, Gudmundur Stefansson, Jaime A. Alvarado-Montes, Corey Beard, Chad F. Bender, Arvind F. Gupta, Samuel Halverson, Shubham Kanodia, Dan Li, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Spin–orbit angles for populations of warm Jupiters (M  p  > 0.75M J and a/R * > 11) and more generally for multiplanet systems. Both figures include only measurements with uncertainties less than 40°. Left: the population of warm Jupiters with measured spin–orbit angles, split by stellar host multiplicity. Those around single stars are overwhelmingly aligned, regardless of their temperature in relation to the Kraft break. Right: the population of planets within multiplanet systems (including nontransiting planets) with measured spin–orbit angles. This population is also overwhelmingly well aligned.
Paper: Time-dependent Dynamics of the Corona
Authors: Emily I. Mason, Roberto Lionello, Cooper Downs, Jon A. Linker, Ronald M. Caplan, Marc L. DeRosa
Figure caption: Left: difference maps showing agreement and disagreement between the steady-state (SS) and time-dependent runs. Black corresponds to locations where the SS is open (negative-polarity CH) but the TDC is closed, medium gray is where both are open (negative polarity), light gray is where the TDC is open (negative polarity) but the SS is closed, white is where both are closed, pink is where TDC is open (positive polarity) but the SS is closed, red is where both are open (positive polarity), and maroon is where the TDC is closed but the SS is open (positive polarity). The blue rectangle on each map shows the region integrated over for Figure 3. Right: 3D visualizations of the same maps at the same times, with the SS field lines in red/orange and the TDC field lines in shades of blue. The seed locations of the field lines are the same for both models, and black lines are open for both SS and TDC.
Paper: Time-dependent Dynamics of the Corona
Authors: Emily I. Mason, Roberto Lionello, Cooper Downs, Jon A. Linker, Ronald M. Caplan, Marc L. DeRosa
Figure caption: (a) Left: forward-modeled emission image for the AIA 211 Å channel at time step 488. Right: the corresponding full-Sun map of AIA 211 Å emission, integrated along the radial direction. The region highlighted in blue is the subregion considered in the second half of this Letter. (b) Plots of B  r  and AIA 211 Å differenced emission; the latter color table highlights where the TDC simulation emission is higher (purple) and where the SS simulations’ emission is higher (orange).
Paper: Time-dependent Dynamics of the Corona
Authors: Emily I. Mason, Roberto Lionello, Cooper Downs, Jon A. Linker, Ronald M. Caplan, Marc L. DeRosa
Figure caption: Comparison of the signed net open fluxes for both cases within the region highlighted with the blue rectangle in Figure 5. This captures the early evolution of the negative-polarity coronal hole; note how rapidly the steady-state cases show open flux in the region of interest during the early emergence of the active region, while the time-dependent case does not reach similar levels for up to 50 hr later.
Paper: Time-dependent Dynamics of the Corona
Authors: Emily I. Mason, Roberto Lionello, Cooper Downs, Jon A. Linker, Ronald M. Caplan, Marc L. DeRosa
Figure caption: (a) Percent of global total open flux for SS and TDC during the selected time period. Except for time step 440, immediately before the emergence of the active region, the SS has uniformly less open flux than the TDC simulation. (b) The global magnetic energy for both the TDC and SS simulations.
Paper: Are There Terrestrial Planets Lurking in the Outer Solar System?
Authors: Amir Siraj
Figure caption: Mass of a captured free-floating planet with an expected abundance of unity in the solar system as a function of maximum semimajor axis. Dashed lines correspond to the 25th and 75th percentile limits.
Paper: Are There Terrestrial Planets Lurking in the Outer Solar System?
Authors: Amir Siraj
Figure caption: Lower panel: cumulative fraction of captured free-floating planets as a function of heliocentric distance. This is independent of planet size. Upper panel: expected number of Earth-, Venus-, Mars-, and Mercury-size planets as a function of heliocentric distance, adopting a nominal albedo of 0.2.
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Flux at 0.89 mm scaled at 160 pc vs. accretion luminosity. Symbols are color-coded by SpTy. The sample of mid-to-late M-star disks includes those in Pascucci et al. (2009), which were only observed at the lowest Spitzer/IRS resolution. Down arrows indicate millimeter upper limits. Triangles are for the mid-to-late M-star disks present in Figure 4, while crosses indicate JWST/MIRI targets. Sz 114 is indicated with a star and shows a significantly higher millimeter flux than other mid-to-late M-star disks observed with Spitzer/IRS.
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Expanded view of wavelength regions covering the ionic, atomic, and molecular lines reported in Table 2. Shaded regions indicate the wavelength ranges over which fluxes are measured. For C2H2 (purple), HCN (red), and CO2 (green), these are the same ranges as those adopted in earlier Spitzer/IRS studies to facilitate comparison with literature sources. For H2O (light blue), the wavelength range is restricted to the complex around 17.22 μm. The best-fit spectra obtained with CLIcK are also shown with solid lines.
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Molecular flux ratios vs. scaled water flux for mid-to-late M-star disks (Pascucci et al. 2013) and disks around earlier-type stars (Banzatti et al. 2020). In these comparisons, the water line at 17.22 μm is adopted. The two downward arrows with a question mark next to them are for the tentative Spitzer water detections in the mid-to-late M-star disks of J043814 and J044427. J160532 is a source similar to Sz 114 in spectral type, stellar mass, and accretion luminosity but is extremely carbon-rich. XX Cha is a slightly earlier-type (M3.5) star with a disk rich in water. Note how Sz 114 (star symbol) has more similar molecular flux ratios to earlier than later SpTy except for CO2/H2O, which is higher than the average earlier-type disk value.
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Reduced MIRI-MRS spectrum of Sz 114 (black). The continuum (red line) is interpolated at the light blue dots and superimposed on the original spectrum. The continuum-subtracted spectrum is shown below in gray. The spectrum is dominated by water emission lines, and wavelengths of other prominent molecular rovibrational bands are indicated as vertical lines. The dips at ∼19, ∼22, and ∼26 μm are not real but rather data reduction artifacts.