adsabs/AstroCLIMB huggingface dataset:
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Kp vs. conjunction time offset the four noninverted planet models with varying metallicity and C/O ratio. All four models show a strong feature consistent with a planet detection at similar Kp and ΔTconj. The peak values correspond to a conjunction time approximately 3 hr before the expectation from G. Hébrard et al. (2016), well within the propagated uncertainty in the conjunction time arising from uncertainty in the orbital period. The peak planet RV semiamplitude is ~167 km s−1 for all models, corresponding to an inclination of 64°. The SNR was calculated by dividing the map by the standard deviation of the Kp < −60 km s–1 region. All models are detected at similar strength.
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Retrieved P−T profile (top left), maximum-likelihood emission contribution function (top right), maximum-likelihood spectrum (middle), and species opacities (bottom). In the P−T plot, the median retrieved profile is shown in green, and the maximum-likelihood profile in purple. The cloud pressures are indicated by horizontal dashed lines. The black lines are the P−T profiles from 500 draws from the retrieved posteriors. In the emission contribution function, spectrum, and opacity panels, the observed orders are shaded in gray. Most of the emission arises between 1 bar and 30 mbar, where the P−T profile begins to cool, and is significantly above the cloud pressure, indicating the atmosphere is clear at the pressures probed by these K-band observations. The maximum-likelihood spectrum shows weak CO features in addition to H2O, and the nondetection of refractory species is consistent with the extremely low opacity of these species in comparison to CO and H2O
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Corner plot showing the retrieved C/O, [C/H], [O/H], and [(C + O)/H] posteriors, computed from the retrieved abundances for H2O and CO. Stellar values are indicated in dashed–dotted blue, while the retrieved median and ±34% confidence intervals are indicated in solid and dotted red, respectively. While the oxygen abundance is subsolar/solar at ~1σ, the carbon abundance is only an upper limit, leading to an upper limit on the C/O ratio. These results are consistent with a metal- and carbon-poor atmosphere for HD 143105 b.
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Kp vs. conjunction time offset the four inverted planet models with varying metallicity and C/O ratio. None of these models give a potential planet detection in the region permitted by the prior ephemeris, indicating the detected planet flux is primarily arising from regions of the planetary atmosphere without a thermal inversion. The peak at Tconj = +2.5 hr, Kp = −175 km s−1 corresponds to a velocity track near transit/inferior conjunction, when the observed disk is dominated by the nightside of the planet. As this is incompatible with the previous ephemeris constraints, and we expect the nightside atmosphere to be noninverted, we believe this feature arises from cross talk with stellar residuals and is not related to the planetary atmosphere.
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Kp vs. conjunction time offset for models of all species, CO, H2O, and Fe + Mg, with abundances based on the noninverted [M/H] = 0.3, C/O = 0.8 model which produced the strongest detection in Figure 1. The conjunction time has been updated based on the measured offsets from Figure 1, so planetary features should appear at approximately Kp = 167 km s−1, ΔTconj = 0 hr. Only H2O is confidently detected. A weak feature is present at the same location with the CO model, but does not dominate the Kp−ΔTconj space and does not constitute an independent detection. The refractory species are not detected.
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Kp−vsys diagrams for the G. Hébrard et al. (2016) ephemeris (left) and the revised ephemeris based on Figure 1 (right). The Z = 0.3, C/O = 0.8, noninverted model was used in both cases. The G. Hébrard et al. (2016) ephemeris produces a detection of comparable strength, but with Δvsys = −60 km s−1, well outside the expected range of offsets for a planet with a well-constrained ephemeris.
Paper: True Mass and Atmospheric Composition of the Nontransiting Hot Jupiter HD 143105 b
Authors: Luke Finnerty, Yinzi Xin, Jerry W. Xuan, Julie Inglis, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Katelyn Horstman, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王
Figure caption: Full corner plot for the six-component retrieval.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Models of spherical envelope with disk and spherical envelope with torus. (a) SED. (b) Decimal logarithm of density section for the model with a disk. the white disk represents the star; the black line is the line of sight. (c) Relative deviation of the model SED from the observed SED. (d). Same as (b) but for the model with a torus.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Corner plot of the posterior probability for parameters of the spherical envelope model obtained using only the SED (Section 5.2). Parameters: ﹩{a}_{{\rm{\max }}}﹩—maximum radius of a dust particle, fC—carbon fraction in dust material, τsph—optical depth in the envelope at λ = 0.5 μm, rin—inner radius of the envelope, b—exponent of envelope density. The rest three parameters characterize the model of SED noise: σ0—amplitude of uncorrelated noise, σc—amplitude of correlated noise, l—noise correlation length.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Left column: correction factor ξ = SEDscat/SEDnoscat for SED, computed at nodes of the grid presented in Table 6. Right column: ratios of SED computed using correction method and by direct account for scattering matrices (Section 5.2.2). Thin color lines stand for a subsample of volume 50 taken from the MCMC-generated sample; the thick black line stands for the optimal model. Upper row: model of the spherical envelope (Section 5.2.2); lower row: model of the spherical envelope and disk (Section 5.3.3).
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Corner plot of the posterior probability for parameters of the model of spherical envelope and disk; the SED and DPV are taken into account (Section 5.2). Parameters: ﹩{a}_{{\rm{\max }}}﹩—maximum radius of dust particles, fC—carbon fraction in dust material, τsph—optical depth in the spherical envelope at λ = 0.5 μm, τdisk—optical depth in the disk equator at λ = 0.5 μm, β—exponent in the dependence of disk scale height on distance from the star, h0—disk scale height at 10 au from the star, ϵ—inclination of the disk.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Modeled images of the system at 880 nm, not convolved by the PSF. Left column: polarized intensity; right column: total intensity. Upper row: model of the spherical envelope (Section 5.2.2); lower row: model of the spherical envelope and disk (Section 5.3.3).
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Same as in Figure 8, but for the optimal model with disk from Section 5.3.3 and for models with disks having β = 0, h0 = 0.7 au and β = 1, h0 = 0.2 au.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Same as in Figure 10, but for models with disks having β = 0, h0 = 0.7 au and β = 1, h0 = 0.2 au.
Paper: Low 4.5 μm Dayside Emission Disfavors a Dark Bare-rock Scenario for the Hot Super-Earth TOI-431 b
Authors: Christopher Monaghan, Pierre-Alexis Roy, Björn Benneke, Ian J. M. Crossfield, Louis-Philippe Coulombe, Caroline Piaulet-Ghorayeb, Laura Kreidberg, Courtney D. Dressing, Stephen R. Kane, Diana Dragomir, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Farisa Y. Morales, David Berardo, Varoujan Gorjian
Figure caption: Joint posterior distribution of the Bond albedo AB (vertical axis) and heat redistribution factor f (horizontal axis) assuming TOI-431 b radiates as blackbody at its 4.5 μm brightness temperature of 1520 K. The 2D posterior is shown using colored shading, where darker regions indicate lower probabilities. The 1σ and 2σ regions are indicated by the black contour lines. The approximate values for the Moon and Mercury are shown in yellow and magenta at the bottom right, respectively.
Paper: Low 4.5 μm Dayside Emission Disfavors a Dark Bare-rock Scenario for the Hot Super-Earth TOI-431 b
Authors: Christopher Monaghan, Pierre-Alexis Roy, Björn Benneke, Ian J. M. Crossfield, Louis-Philippe Coulombe, Caroline Piaulet-Ghorayeb, Laura Kreidberg, Courtney D. Dressing, Stephen R. Kane, Diana Dragomir, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Farisa Y. Morales, David Berardo, Varoujan Gorjian
Figure caption: Best-fitting white-light curve from the analysis of the seven eclipses of TOI-431 b with Spitzer Channel 2. The eclipse light curve generated from the average eclipse depth of 33 ppm is shown in the black line, with ±1σ and ±2σ ranges shown in gray. The blue circles represent the individual systematics-corrected observations and their associated error bars. The Spitzer data points are binned to 8.33 minutes intervals, and the bold black points represent the combination of all the data binned by groups of 250 points. The first and last 45 minutes of each data set have been removed.
Paper: Low 4.5 μm Dayside Emission Disfavors a Dark Bare-rock Scenario for the Hot Super-Earth TOI-431 b
Authors: Christopher Monaghan, Pierre-Alexis Roy, Björn Benneke, Ian J. M. Crossfield, Louis-Philippe Coulombe, Caroline Piaulet-Ghorayeb, Laura Kreidberg, Courtney D. Dressing, Stephen R. Kane, Diana Dragomir, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Farisa Y. Morales, David Berardo, Varoujan Gorjian
Figure caption: Measured eclipse depths for all seven visits using three different systematic models, including the associated error bars of each. The rightmost points show the weighted average across all visits for the individual systematics.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Top left: longitude–velocity (l–v) map, integrating over Galactic latitude b = −0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩464–0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩536. Bottom left: longitude–latitude (l–b) map, integrating over velocity Vlsr = 70–125 km s−1. Bottom right: velocity–latitude (v–b) map, integrating over Galactic longitude l = 24﹩\mathop{.}\limits^{\unicode{x000B0}}﹩099–25﹩\mathop{.}\limits^{\unicode{x000B0}}﹩099. Blue, green, and red colors in all maps represent regions where 12CO, 13CO, and C18O emission were detected, respectively. In the l–v and v–b maps, there are two distinct velocity components, 30–65 km s−1 and 70–125 km s−1, the latter of which is the object of our study. Based on the distribution characteristics of C18O, we selected seven subregions for comparison and set the size of subregion A to 16′ × 16′, the size of subregions B, C, and D to 8′ × 8′, and the size of subregions E, F, and G to 4′ × 4′.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Spatial distributions of 12CO (top), 13CO (left), and C18O (right) clumps. The background gives integrated intensity maps of the corresponding CO and its isotopes' emission. The ellipses denote the positions of the clumps, where the cyan ellipses do not have the potential to form massive stars and the red ellipses indicate potential formation sites for massive stars, as detailed in Section 4.1.5.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: The relationship between XCO and ICO. Left panel: each black dot represents a voxel, which detects both 12CO and 13CO. Right panel: each black dot represents a pixel that integrates over all velocity channels where 12CO emission is detected, regardless of whether 13CO emission is detected or not. The contours outline the surface densities of the black dots. The median and mean values of XCO are indicated in the lower left of each panel.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Cumulative distribution functions of the peak main-beam temperatures (Tpk), excitation temperature (Tex), H2 column density (﹩{N}_{{{\rm{H}}}_{2}}﹩), and mass (M) of the 12CO, 13CO, and C18O emission for the seven subregions.The first to fourth rows are Tpk, Tex, ﹩{N}_{{{\rm{H}}}_{2}}﹩, and M, respectively, and the first to third columns denote the physical quantities of the 12CO, 13CO, and C18O emission, respectively.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: The HCO+ (violet) emission region and the 12CO (blue), 13CO (green), and C18O (red) emission regions from 78 to 124 km s−1, with corresponding HCO+ spectral line profiles. Upper panel: integrated intensity map for velocities from 78 to 124 km s−1 for contours of 20%, 50%, and 80%, with the 12 regions with HCO+ emission labeled 1–12. Lower panel: HCO+ spectral line profiles corresponding to the 12 regions.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: An infrared image of the Herschel 70 μm band (S. Molinari et al. 2010), with central coordinates l = 24﹩\mathop{.}\limits^{\unicode{x000B0}}﹩599 and b = +0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩036, with an image size of 1∘ × 1∘. The red boxes mark the locations of three MSFRs.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: The average spectra of the G24 region and its seven subregions. Note that only pixels with intensities ≳×  · σ in at least three consecutive channels are averaged. X = 11 for 12CO and 13CO, and X = 7 for C18O.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Upper left: map of Tex distribution. Upper right: map of ﹩{N}_{{{\rm{H}}}_{2},12}﹩ distribution. Lower left: map of ﹩{N}_{{{\rm{H}}}_{2},13}﹩ distribution. Lower right: map of ﹩{N}_{{{\rm{H}}}_{2},18}﹩ distribution. Subregions A–G are labeled on each of the four maps.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: A comparison of the abundances of various COMs relative to CH3OH across different sources, including V883 Ori, is presented in this work. The abundances relative to CH3OH for the different sources were compiled from the literature as follows: for IRAS 16293 A and B, values are from S. Manigand et al. (2020), H. Calcutt et al. (2018), S. Manigand et al. (2019), and P. Nazari et al. (2024); for the protostar B1-c, from M. L. van Gelder et al. (2020) and P. Nazari et al. (2021); for the protoplanetary disk IRS 48, from N. G. C. Brunken et al. (2022); for the comet 67P/C-G, from N. Hänni et al. (2023) and M. N. Drozdovskaya et al. (2018); and for Sgr B2(N), from A. Belloche et al. (2013). The red downward arrow in the source IRS 48 indicates the upper limit due to nondetection.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Comparison of N-bearing species relative to ﹩{{\rm{CH}}}_{3}{\rm{CN}}﹩ in low- and high-mass protostars. The abundances are compiled from the literature as follows: Sgr B2(N) from A. Belloche et al. (2013), 101899 and 126348 from P. Nazari et al. (2022), B1-c and S68N from P. Nazari et al. (2021), and IRAS 16293 A and B from H. Calcutt et al. (2018), S. Manigand et al. (2020), N. F. W. Ligterink et al. (2017), and S. Zeng et al. (2019). The black downward arrow indicates the upper limit due to tentative detection. For HNCO, NH2CHO, ﹩{{\rm{CH}}}_{3}{\rm{OCN}}﹩, and CH3NCO in IRAS 16293 A, the column density of ﹩{{\rm{CH}}}_{3}{\rm{CN}}﹩ is adopted from H. Calcutt et al. (2018).
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Comparison of various COM abundances relative to methanol (CH3OH) in V883 Ori from this study with those in Y. Yamato et al. (2024, Band 3 observations), J.-E. Lee et al. (2019b, Band 7 observations), and J.-E. Lee et al. (2024, Band 6 observations). The red downward arrow indicates an upper-limit column density.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: The three categories of Tex for different molecular species. The first category includes molecules with low Tex, shown in blue (Tex ∼ 50–100 K). The second category represents warm species (Tex ∼ 100–200 K), shown in orange, and the third includes hot molecules (Tex ∼ 200–400 K), shown in red. We only plotted molecules for which Tex is well constrained by the model.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: Identified COMs toward the disk of V883 Ori. The horizontal dotted line in gray represents the noise level in the data (1σ), the black line represents the data, and different colors represent the best fit of the model of different species.
Paper: A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van 'T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, Jenny K. Calahan
Figure caption: In blue is the simulated intensity at Tex = 100 K and Ntot = 3 × 1016 cm−2 of the three transitions of HDCO that are detectable under the physical conditions of this source. The red vertical lines indicate the central frequency of each transition.