adsabs/AstroCLIMB huggingface dataset:
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Light and color curves of CSS 161010. Top: UV and optical light curves of CSS 161010. Upper limits are presented as open symbols. The start of the outburst is indicated by a vertical black arrow. The vertical magenta lines are the epochs of optical spectroscopy. The photometry is host-subtracted (except in the I band) and corrected for Milky Way extinction. Bottom: intrinsic color curves of CSS 161010.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Top panels: CSS 161010 g-band (left), r-band (middle), and bolometric light curves (right) compared with the well-sampled LFBOT AT 2018cow (purple circles); SNe with hydrogen in their spectra: SN 1979C (SN II), SN 2008es (superluminous SN II); and three hydrogen-rich TDE candidates: AT 2018zr, AT 2020neh, and AT 2020wey. In the g-and r-band light-curve comparisons, the LFBOTs with good optical coverage, AT 2020mrf (yellow downward-facing triangles) and AT 2020xnd (green pentagons), are also included. The CSS 161010 V-band light curve is also shown (thick gray line; left panel). Details of the comparison sample are presented in Table F1. Bottom panels: g − r colors (left), blackbody temperature (middle), and blackbody radius (right) of CSS 161010 compared with SN 1979C, SN 2008es, AT 2018cow, AT 2018zr, AT 2020neh, and AT 2020wey. JD = 2457669.92 ± 2.00 is the start of the outburst estimated for CSS 161010.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Correlation between the BH mass and TDE light-curve decay time (S. van Velzen et al. 2020). The dashed blue line shows the expected relation between t fb and M BH for a star of 1 M *. This line is extended (light blue) to lower values. The red star marks the location of CSS 161010 obtained by extending the t fb and M BH correlation. The red rectangle shows the uncertainty obtained from the light-curve fitting (Appendix D, Figure D1). Purple stars show the BH masses obtained from the M * and M BH relations (Figure 1; Appendix B). Reproduced and modified from S. van Velzen et al. (2020).
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Left panels: spectral comparison of CSS 161010 with the AT 2018cow-like objects: AT 2018cow, AT 2020xnd, and AT 2020mrf at different epochs. Middle panels: spectral comparison of CSS 161010 with fast-declining hydrogen-rich events: SNe 1979C and 2008es and the TDE candidates AT 2018zr, AT 2020neh, and AT 2020wey. Each spectrum has been shifted in flux for comparison. The vertical dashed lines indicate the rest wavelength positions of a selection of spectral lines. Right panels: CSS 161010 Hα profile in velocity space compared with AT 2018cow (top) and the fast-declining hydrogen-rich SN 1979C and the TDE candidates AT 2018zr, AT 2020neh, and AT 2020wey (bottom). Vertical dashed lines in the middle and right panels mark the velocities at −20,000, −10,000, 0, and 10,000 km s−1.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Fit results from PROSPECTOR obtained for the photometric SED (upper left) and spectroscopic SED (upper right) of CSS 161010’s galaxy; red lines and points show the best model (maximum a posteriori, or MAP), while the orange lines show 100 random samples of the posterior. The corner plot shows the sampling of the posterior probability distribution for the parameters obtained using PROSPECTOR (excluding the star formation history amplitudes). The middle right plot shows the nonparametric star formation history inferred through eight age bins. The median and 16th and 84th percentiles of CSS 161010’s host parameters are shown in Table B1.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Bolometric light curve of CSS 161010. The dashed lines indicated the best fit for ﹩{\left({t}/{{t}}_{0}\right)}^{p}﹩ with p as a free parameter (blue) and p = –5/3 (red). Solid lines (red and blue) show 100 random samples of the posterior by using Markov Chain Monte Carlo.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Comparison of the Hα (black) and Hβ (cyan) profiles from 21.0 to 57.7 days from the start of the outburst. The phases are labeled on the top of each panel. The vertical dashed lines mark the velocities at −30,000, −20,000, −10,000, 0, and 10,000 km s−1. To match both profiles, we multiplied Hβ by 3 in the first four panels and by 2 in the last two.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Lines identified in the spectra of CSS 161010 at ∼10.4 and ∼27.9 days after the start of the outburst. The dashed lines indicate the rest position of the helium (top) and hydrogen (bottom) lines. The shaded regions mark their blueshifted locations.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Location of CSS 161010 within its host galaxy. Images obtained by ALFOSC on the NOT showing the transient (top), the host galaxy when the transient had faded away (middle), and subtracted difference images (bottom). B-band images are shown in the left panels, while V-band images are on the right.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Evolution of the EW (panel (a)), velocity offset (i.e., blueshift of the line peak from the rest wavelength; panel (b)), FWHM velocity (panel (c)), highest velocity (panel (d)), and luminosity (panel (e)) of the Hα  profile from 21.0 to 57.7 days.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Column density for H2O, CO2, and C2H2 as a function of radius for the models in Table 4. The color bar reflects the value of C/O for each model, and the linestyle indicates the method for increasing the C/O ratio. The dashed–dotted horizontal line shows the best-fit value found from LTE slab models, along with the shaded 1σ uncertainty. The shaded gray vertical region corresponds to the emitting area estimated from slab models. In the case of CO2, we assumed this value to be an annulus of the same area instead of a continuous distribution, and we placed the ring where it best matched the thermochemical models.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: The top row shows the column density predictions from the thermochemical models for C2H4, C2H6, and C6H6. The bottom row shows slab models that simulate the conditions predicted by the thermochemical calculations. The parameters used for each slab model are listed in the figure. Two sets of slab models were tested, one cospatial with C2H2 (orange) and one cospatial with C4H2 (green). These models (green and orange) are shown on top of the data (black) in the bottom left. The pink-shaded region in the bottom right panel corresponds to the same composite model as in Figure 2.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Gas (top) and dust (bottom) temperature profiles from the thermochemical models. The colored contours in the top figure represent the contribution functions for the water_dep_co model (see Table 4), where 90% of the emission is produced. The transitions for each molecule are indicated in Table 5. The lines in the bottom plot represent the 250 K and 500 K contours, inside of which we change the abundances to increase the C/O ratio.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Contribution function-weighted temperatures of carbon and oxygen-bearing species for the water depletion models. The symbols represent where in the model the C/O ratio is changed, inside T = 250 K or T = 500 K. The markers are shifted horizontally for clarity. For comparison, we include the temperature retrieved from slab models as a black square, with errors corresponding to the 1σ uncertainty.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Continuum-subtracted spectrum and best-fit slab models for the molecules detected. The data were offset vertically for clarity. The pink-shaded region shows the composite model of C2H2, 13C12CH2, HCN, CO2, H2O, C4H2, and HC3N. We show a closer look at the HC3N feature in Figure 12.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Gas (top) and dust (bottom) density profiles from the thermochemical models. The orange line in the bottom plot shows the continuum τ = 1 line at 15 μm. Inside 10 au, the large dust population is mostly settled in the midplane.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: JWST MIRI-MRS spectrum of DoAr 33. The insets show isolated emission features of some of the molecules detected, and the calculated continuum is shown as a pink line. Most of the unmarked emission lines correspond to water vapor. We discuss the presence of dust emission features in Appendix A.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Same as Figure 5, but for C4H2.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Grids of χ 2 for the molecules fitted with LTE slab models. The color scale shows the reduced χ 2, the white contours show the 1σ, 2σ and 3σ  uncertainty levels and the dashed black contours correspond to the best-fit emitting radius for each pair. The bottom panel right corresponds to the 13C12CH2 fit, where the temperature and emitting area are fixed to that of C2H2; therefore, we fit only the column density.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: SED fits of the radiative transfer models using RADMC-3D. The input stellar UV flux for DoAr 33 is reduced relative to AS 209 for wavelengths <0.22 μm. The best-fit model is shown as the solid black line, and the other models are shown in light gray. The inset shows the fit to the MIRI-MRS spectrum.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: C2H2 to water fraction for disks surrounding a range of stellar masses and accretion rates. The gray points are taken from C. F. Manara et al. (2023). The colored points have JWST MIRI observations and column density estimates. The color indicates the ratio of the C2H2/H2O column. The empty solid-line points report no C2H2 detection, and the empty dotted-line points report no H2O detection. The dashed line corresponds to ﹩\dot{M}\propto {M}_{\star }^{2}﹩.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Dust features present in the MIRI-MRS spectra of DoAr 33. The Spitzer observations are taken from E. Furlan et al. (2011) and have been scaled to match the peak of the 10 μm feature. The dust opacities from optool are shown for reference and have also been scaled.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Tentative detection of CH4 in the MIRI-MRS spectrum of DoAr 33. The top spectra show the best-fit slab model of C2H2 in orange, along with an H2O model in blue, with parameters indicated in the text. The MIRI spectra in the top and middle were offset for clarity. The green line shows the best-fit CH4 slab model, and the bottom pink spectrum shows the composite model of the three species.
Paper: JWST/MIRI Detection of a Carbon-rich Chemistry in the Disk of a Solar Nebula Analog
Authors: María José Colmenares, Edwin A. Bergin, Colette Salyk, Klaus M. Pontoppidan, Nicole Arulanantham, Jenny Calahan, Andrea Banzatti, Sean Andrews, Geoffrey A. Blake, Fred Ciesla, Joel Green, Feng Long, 凤 龙, Michiel Lambrechts, Joan Najita, Ilaria Pascucci, Paola Pinilla, Sebastiaan Krijt, Leon Trapman
Figure caption: Tentative detection of HC3N in the spectrum of DoAr 33. The bottom spectrum shows the individual models for each molecule, the pink spectrum in the middle shows the composite model when HC3N is included, and the top green spectrum shows the composite model when HC3N is not included.