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Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Summary of stellar and disk properties for 30/31 JDISCS targets included in this work, including mass accretion rates (y-axis), submillimeter dust disk radii enclosing 90%–95% of the flux at ∼1.3 mm (x-axis), and stellar masses (marker colors). The sample spans ∼4 orders of magnitude in mass accretion rate, ∼2 orders of magnitude in dust disk sizes, and a narrow range in stellar masses (27 K- and M-type T Tauri stars, one G-type star, and three Herbig Ae/Be systems). AS 205 S is excluded from the figure, as it does not yet have a measured accretion rate.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Color–magnitude diagram from 2024 November 25, showing alerts from the night of 2024 November 24. Alert data points are plotted in front of a 2D histogram color–magnitude diagram of the Gaia catalog of nearby stars. Objects that passed all filter constraints from the SQL query posed via the Lasair API are plotted as orange squares. Objects that passed both the initial Lasair filter and the second round of statistical tests and other constraints beyond the brokers are plotted as purple stars. The letters correspond to the ZTF object names associated with each purple star: A for ZTF24abbldyz, B for ZTF24abjinpg, C for ZTF24abgzfsz, and D for ZTF24ablvgno. Note that point D is partially obstructed by the yellow diamond. Although not from the night of 2024 November 24, we plot ZTF24aaerzwh, our curious long-period variable, as a yellow diamond. This long-period variable is clearly situated on the main sequence.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Light curve for ZTF24aaerzwh. This source was crossmatched by Lasair with 4479767064322208640, a G = 13.40 mag stellar source found in the Gaia and PS1 catalogs. The source has been classified in the ZTF catalog of periodic variable stars as a BY Draconis variable. The data plotted are an amalgamation of historical data pulled from the ZTF archive and alert-packet data pulled with the Lasair API query. R-band and G-band data are shown in red and blue, respectively. Data pulled from the ZTF alert packet are plotted in a darker shade. This alert-packet data are also distinguished from archival data because they lie to the right of the alert-epoch line, indicating the object’s discovery date in Lasair. The right-most dotted line indicates the “MJD min” or 30 days before the object’s most recent alert.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Light curves are plotted for all four objects that passed both sets of filters within and beyond the brokers on the night of 2024 November 24. Left to right and top to bottom, we have ZTF24abbldyz, ZTF24abjinpg, ZTF24abgzfsz, and ZTF24ablvgno. Figure 7 shows these objects plotted on a color–magnitude diagram as points A, B, C, and D, respectively. As in Figure 4, the data plotted are an amalgamation of historical data pulled from the ZTF archive and alert-packet data pulled with the Lasair API query. I-band, R-band, and G-band data are shown in purple, red, and blue, respectively. Note that I-band data are the least represented of the three bands, thus we primarily use R-band and G-band data to draw conclusions about the objects’ behavior. All other plot features are the same as in Figure 4. It can be observed in all four light curves that the alert-packet data are fainter than the historical data, indicating a dip in brightness. ZTF24abbldyz shows a gradual dip in brightness beginning well before the alert epoch (≈250 days earlier) and continuing until the most recent data. Despite having noisier data, ZTF24ablvgno shows a clear dip in brightness beginning roughly 500 days before the alert epoch.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Simulated dips of varying amplitudes are plotted along with g-band data from ZTF24abbldyz. Simulated dips are plotted in color, where each color indicates a different amplitude. Real data for ZTF24abbldyz are plotted in gray scale. The horizontal dotted line indicates the median magnitude of historical g-band for ZTF24abbldyz data at least 100 days older than the object’s discovery date in Lasair. The solid vertical line marks this discovery date, and gray points plotted to the right of the line are included in the object’s ZTF alert packet. We plot simulated dips in 0.01 mag increments ranging from 0 to 0.2 mag. We use our simulated data to perform the two-sample K-S test and investigate how the p-value depends on the dip amplitude.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: p-value from the two-sample K-S test is plotted against simulated dip depth for ZTF24abbldyz, where the color corresponds to dip magnitude as in Figure 5. The horizontal red line indicates a p-value of 0.05, the cutoff for our two-sample K-S test with a 95% confidence interval. The p-value for the actual alert data is starred. As expected, the p-value decreases with dip amplitude and the relationship appears exponential. The 0.05 p-value cutoff successfully eliminates candidates with dip amplitudes close to zero and recognizes dip amplitudes greater than about 0.01 mag as statistically significant.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Transit zones for all solar system planets are plotted in heliocentric ecliptic coordinates (left) and in celestial coordinates (right). Each planet’s transit zone is shown as a colored sinusoidal band. Sensors located in the colored regions of sky could detect the corresponding planets as they transit the Sun. Overlaps between colored bands indicate regions where multiple planets could be detected. Note there are 28 regions of overlap between sets of two planet transit zones and eight regions of overlap for sets of three planets. We adapt code from R. Wells et al. (2018) and use the updated transit zone geometry (Figure 1) to calculate and plot the full transit zone angles as ϕTZ = ﹩2\arcsin (({R}_{\odot }-{R}_{{\rm{p}}})/r)﹩.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: SSP contributions for each star cluster from the STARLIGHT results. From upper left to bottom right: NGC 1711, NGC 1718, NGC 1801, NGC 1806, NGC 1818, NGC 1849, NGC 1866, NGC 1916, SL 505, NGC 2100, NGC 2136, and NGC 2137. In orange the SSP, in blue and light blue are the weighted average log(age), (﹩\overline{{\mathrm{log}}\,({t}_{w}(\mathrm{yr})})﹩, and the log of weighted average age, (﹩{\mathrm{log}}\,(\overline{{t}_{w}(\mathrm{yr}))}﹩), respectively. The size of the orange circles means the contribution rate of each SSP.
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: MOC map for the Mercury transit zone is plotted in purple with a HEALPix cell resolution of 12. The plot is a projection of the world coordinate system to the pixel image coordinate system. The right-hand plot more clearly shows the jagged edge of the MOC rendering, which slightly overestimates the total transit zone region.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The main Sorcha workflow. Sorcha is split into two stages. The ephemeris generation stage (described in Section 6) is in gray, and the postprocessing stage (described in Section 7) is in green and magenta. We note for the reader that this workflow is for simulating what the LSST is expected to discover. We note there are a small number of additional functions/filters available (described in Section 7.11) that can be applied to produce different desired outputs of the simulated small body detections and discoveries based on the user’s desired science case.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The trailing of moving solar system objects visualized with Dark Energy Survey (DES; T. M. C. Abbott et al. 2021) observations. The top two rows show the image cutouts and PSF (point-spread function) contours of example solar system objects (identified by the red crosshairs in the cutouts). The last row shows the PSF contours for representative reference stars within the same images. Slow-moving TNO (20000) Varuna has a stellar-like PSF (shown on the left) and fast-moving NEO (65803) Didymos has an extended significantly trailed PSF, as shown on the right. Dark Energy Camera (DECam; B. Flaugher et al. 2015) data was selected because of the expected similarity to the LSSTCam images (Ž. Ivezić et al. 2019; F. B. Bianco et al. 2022).
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: A cartoon schematic depicting the difference between how the trailed source magnitude and the PSF magnitude for a moving solar system object observed on an LSST image are estimated. The Rubin Data Management source detection pipeline, the Difference Image Analysis (DIA) pipeline, uses PSF filter matching to find sources on the image. This pipeline will measure the PSF magnitude. Only transient sources identified by the DIA pipeline will be sent on to the Rubin Solar System Processing (SSP) pipelines to search for moving objects. The SSP pipelines will report the trailed source magnitude.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The LSSTCometActivity class’s cometary activity model included in the Sorcha add-ons package is demonstrated here. The apparent magnitude (trailed source magnitude) in the r band as a function of heliocentric distance is plotted for an inactive comet nucleus (black) and an active comet (Afρ1 = 150 cm and k = −0.3.). Both simulated objects have a nucleus of Hr = 17. No phase function effects are included in order to highlight the impact from cometary activity(α = 0 is assumed at all distances).
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: Demonstration of the difference between the trailed source magnitude and the PSF magnitude. We plot the reduced magnitude derived from the PSF magnitude (blue dots) and the trailed source magnitude (red curve), simulated for asteroid (24) Themis. The PSF magnitude measures less flux because it is not sampling using the full image trail from the simulated detection, and therefore, a clear flux loss can be seen in the reduced PSF magnitude, which varies with the on-sky velocity of Themis, compared to the reduced magnitude calculated from the trailed source magnitude. For any photometric analyses of simulated detections/discoveries output by Sorcha, the user should use the reported trailed source magnitude.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The effects of the simple sinusoidal light-curve model included in the Sorcha add-ons package for different phase function models. The dashed lines show the unmodified apparent magnitude (trailed source magnitude); the solid lines show the apparent magnitude after the model has been applied.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: Sorcha inputs and outputs. This figure provides an overview of the input files that are ingested by Sorcha and the possible resulting simulation outputs.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: MRS continuum-subtracted spectra of C2H2 (magenta), HCN (green), H2O (blue), and CO2 (brown) emission lines between 13.6 and 15.3 μm from JDISCS sources with submillimeter dust sizes r > 63 au. ALMA images are shown to the right of the spectra (S. M. Andrews et al. 2018; F. Long et al. 2018, 2019; F. Long et al. 2025, in preparation), in order of submillimeter dust disk size from largest (top left; Elias 27, r ∼ 250 au) to smallest (bottom right; RU Lup, r ∼ 63 au). Slab model fits to the molecular emission lines are overplotted on the spectra, corresponding to the best-fit parameters and upper limits reported in Tables 5, 6, 7, and A1. 13C12CH2 emission is also detected in the spectrum of GO Tau, along with multiple CO2 isotopologues in MY Lup (C. Salyk et al. 2025), and an OH-rich spectrum with no CO2 emission from GM Aur (C. E. Romero-Mirza et al. 2025, in preparation).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: MRS continuum-subtracted spectra of C2H2 (magenta), HCN (green), H2O (blue), and CO2 (brown) emission lines between 13.6 and 15.3 μm from JDISCS sources with submillimeter dust sizes r < 60 au. ALMA images are shown at the right (S. M. Andrews et al. 2018; F. Long et al. 2018, 2019; F. Long et al. 2025, in preparation), in order of submillimeter dust disk size from largest (top left; AS 205N, r ∼ 60 au) to smallest (bottom right; GK Tau, r ∼ 13 au). Slab model fits to the molecular emission lines are overplotted on the spectra, corresponding to the best-fit parameters and upper limits reported in Tables 5, 6, 7, and A1. 13C12CH2 emission is also detected in the spectrum of DoAr 33 (M. J. Colmenares et al. 2024).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Emission-line luminosities from best-fit slab models (integrated between 12 and 16 μm) vs. peak-to-continuum values from the slab models and fit to the continuum, with marker styles indicating the spatially resolved submillimeter structures in Table 2. Targets in the upper-right quadrant show the clearest molecular gas detections, and we report nondetections (red markers) when peak-to-continuum ratios are <0.03 or emission-line luminosities are smaller than ﹩{\mathrm{log}}\,L\lt -5.1\,{L}_{\odot }﹩ (black, dashed lines). While disks with resolved submillimeter dust cavities show C2H2 and HCN emission lines, none of these sources have CO2 emission.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Retrieved temperatures from slab model fits to C2H2 (top, magenta), HCN (middle, green), and CO2 (bottom, brown) emission lines from JDISCS sources in order of decreasing submillimeter disk size from top to bottom of each panel. Vertical dashed lines and shaded regions represent the sample median ±1σ, with red x’s along the median lines denoting nondetections for each molecule. Black markers identify the submillimeter substructures, as listed in Table 2. The C2H2 and HCN temperatures are generally consistent, while the CO2 is cooler.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Gallery of rovibrational CO, OH, [Ne II], and [Ne III] emission lines from 30/31 JDISCS sources (HD 163296 is excluded due to poor data quality). The spectra are in order from largest to smallest submillimeter disk size, with representative slab models of H2O overplotted on the data surrounding the [Ne II] and [Ne III] emission lines (following A. Banzatti et al. 2025). C2H2 and HCN slab models are shown as well, with the same color scheme as in Figure 3.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Emission-line luminosities (left) and emitting masses (right) integrated from slab model fits to C2H2, HCN, and CO2 between 12 and 16 μm in JDISCS sources. Despite spanning a limited range in stellar masses, the targets display at least an order of magnitude variation in mid-infrared luminosity and mass of each molecule. Violin widths represent the number of disks with detections of each molecule, such that narrower violins correspond to lower detection rates.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Left panel: example corner plot, showing the strong degeneracy between column density and slab radius in LTE slab model fits to the C2H2 emission from AS 205N. The effect is still apparent when HCN and CO2 emission lines are included in the fit. Right panel: degenerate slab model solutions overlaid on JDISCS spectrum of AS 205N.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Median emission-line luminosities from C2H2 (left), HCN (middle), and CO2 (right) vs. the median slab temperatures measured from the 100 best-fit slab models for each disk, with markers representing the submillimeter dust substructures listed in Table 2. The slab temperatures and emission-line luminosities are not correlated for any of the three molecules (Spearman ρ = 0.006, 0.07, −0.1; p = 0.9, 0.8, 0.6, respectively), implying that brighter emission lines do not necessarily originate in hotter gas.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Detection rates of CO, H2O, HCN, C2H2, CO2, and OH for K and M stars in this sample of MRS spectra. Hatches show IRS or ground-based (for CO) detection rates from K. M. Pontoppidan et al. (2010). Earlier spectral types are excluded from this plot due to low number statistics in the JDISCS sample.