adsabs/AstroCLIMB huggingface dataset:
Paper: The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN
Authors: Yutian Chi, Chenglong Shen, Junyan Liu, Zhihui Zhong, Mathew Owens, Christopher Scott, Luke Barnard, Bingkun Yu, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Yuming Wang, Tielong Zhang, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Mengjiao Xu, Long Cheng, Zhenpeng Su, Dongwei Mao, Zhiyong Zhang, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Mike Lockwood
Figure caption: Panel (a) shows the magnetic field strength and the r, t, n components in the RTN coordinate of ICME-1 at BepiColombo. The lavender vertical line and lavender shaded area represent indicate the arrival of the shock and interval of ICME-1. The red vertical line shows the predicted arrival time of ICME-1. Panel (b) shows Tianwen and MAVEN spacecraft in situ observations of a 5 day time interval starting from 00:04UT on 2021 December 8. From top to bottom, these panels are the magnetic field strength (B), the elevation (θ) and azimuthal (ϕ) angles of the magnetic field in the MSO coordinate system, three components of the magnetic field in the MSO coordinate system (B x , B y , and B z ) from MAVEN/MAG (black asterisks) and Tianwen-1/MOMAG (red asterisks), solar wind speed (Vsw), proton density (N p ), the total pressure(Pdp), proton temperature (T p ), and plasma beta (β) from MAVEN/SWIA. The blue solid line represents the simulated solar wind velocity with the ICME calculated from the HUXt model. The lavender vertical line and lavender shaded area represent the shock caused by the ICME and interval corresponding to the ICME determined from the data, while the red vertical line indicates the projected arrival time from the HUXt model.
Paper: The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN
Authors: Yutian Chi, Chenglong Shen, Junyan Liu, Zhihui Zhong, Mathew Owens, Christopher Scott, Luke Barnard, Bingkun Yu, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Yuming Wang, Tielong Zhang, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Mengjiao Xu, Long Cheng, Zhenpeng Su, Dongwei Mao, Zhiyong Zhang, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Mike Lockwood
Figure caption: Panel (a) shows the magnetic field measurements of the ICME at BepiColombo. Panel (b) shows Tianwen and MAVEN spacecraft in situ observations of a 4 day time interval starting from 00:01UT on 2021 December 28. The plot setup is the same as in Figure 2.
Paper: First Detection of a Linear Structure in the Midplane of the Young HH 211 Protostellar Disk: A Spiral Arm?
Authors: Chin-Fei Lee, Kai-Syun Jhan, Anthony Moraghan
Figure caption: ALMA continuum maps toward the center of the HH 211 protostellar system at ∼352 GHz. The cross marks the position of the central protostar. The red and blue arrows indicate the axes of the redshifted component and blueshifted component of the jet axis, respectively. Panel (a) shows the continuum map at a resolution of 0.″040 × 0.″025. The contours start at 5σ with a step of 4σ, where σ = 0.54 K. Panels (b)–(d) show the continuum map at a resolution of 0.″022 × 0.″013. Panel (c) also shows SiO J = 8–7 intensity maps (contours) of the jet at high velocity in order to determine the jet base (as marked by an “x”) near the central protostar. The SiO maps have a resolution of 0.″029 × 0.″018. Blue contours show the blueshifted emission integrated from V off ∼ −34 to −21 km s−1, while red contours show the redshifted emission integrated from V off ∼ 21 to 34 km s−1, where V off = V LSR − V sys, with the systemic velocity V sys = 9.1 km s−1. The contours start from 3σ with a step of 1σ, where the noise level σ ∼ 120 K km s−1. The dotted curves show the limb-brightened edges of the jet. Panel (d) also shows the cyan dotted lines to indicate the three linear structures detected in the disk. An unsharp masking filter has been applied to the continuum map to increase the map contrast. The curved arrows indicate the rotation direction of the disk.
Paper: First Detection of a Linear Structure in the Midplane of the Young HH 211 Protostellar Disk: A Spiral Arm?
Authors: Chin-Fei Lee, Kai-Syun Jhan, Anthony Moraghan
Figure caption: The model maps, simulated maps, and residual maps from our models. Residual maps are obtained by subtracting the model visibility from the observed visibility, with the gray and cyan contours for the positive and negative residuals, respectively. The contours start from 4σ with a step of 3σ, where σ = 1.6 K. Left column shows the maps for the disk model without a pair of trailing spiral arms in the midplane. Central column shows the maps for the disk model with a pair of trailing spiral arms in the midplane. Right column shows the maps for the disk model with a pair of slightly less-inclined trailing spiral arms in the midplane.
Paper: First Detection of a Linear Structure in the Midplane of the Young HH 211 Protostellar Disk: A Spiral Arm?
Authors: Chin-Fei Lee, Kai-Syun Jhan, Anthony Moraghan
Figure caption: Disk models to produce the dust emission in the HH 211 disk. (a) A disk model without a pair of spiral arms in the midplane of the disk tilted at the observed inclination angle. (b)–(d) A disk model with a pair of spiral arms in the midplane. (c) Color range is changed to start from 40 K in order to reveal the spiral arms in the inner disk. (d) The disk is face on in order to reveal the spiral arms in the whole disk.
Paper: First Detection of a Linear Structure in the Midplane of the Young HH 211 Protostellar Disk: A Spiral Arm?
Authors: Chin-Fei Lee, Kai-Syun Jhan, Anthony Moraghan
Figure caption: Toomre Q values for our simple model with a pair of trailing spiral arms in the midplane.
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Results of the MCOS analysis, which prefers a model including both HD and monopole correlations. Top: MCOS S/N for HD correlations (solid blue) and monopole correlations (dashed orange), marginalized over CURN 13/3 noise parameter posteriors. The vertical lines indicate the mean S/Ns. We find S/Ns of 3.4 ± 0.8 for HD correlations and 2.9 ± 0.8 for monopole correlations. Bottom: binned cross-correlations ρ  ab  (black error bars), computed with MAP noise parameters from a CURN 13/3 run. The solid blue and dashed orange curves show best-fit HD and HD+monopole correlation patterns, corresponding to ﹩{\hat{A}}^{2}=6.8\times {10}^{-30}﹩ and to ﹩{\hat{A}}_{\mathrm{HD}}^{2}=5.5\times {10}^{-30}﹩, ﹩{\hat{A}}_{\mathrm{monopole}}^{2}=8\times {10}^{-31}﹩, respectively. The monopolar component accounts for the vertical shift of the cross-correlations with respect to the HD curve. We use the standard version of the optimal statistic that does not include interpulsar correlations to compute ρ  ab , so the points and errors do not match those shown in Figure 1(c).
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Empirical background distribution of HD  γ -to-CURN  γ  Bayes factor (left; see Section 3) and noise-marginalized optimal statistic (right; see Section 4), as computed in 5000 sky scrambles, which erases the dependence of interpulsar correlations on the angular separation between the pulsars. Dotted lines indicate Gaussian-equivalent 2σ, 3σ, and 4σ thresholds. The dashed vertical lines indicate the values of the detection statistics for the unscrambled data set. We find p = 1.6 × 10−3 (~3σ) for the Bayesian analysis and p < 10−4 (>3σ) for the optimal statistic analysis.
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Comparison between empirical background distributions for the noise-marginalized optimal statistic, as computed by the sky scramble technique. We show distributions computed using a match threshold of ﹩\bar{M}\lt 0.17﹩ (blue), ﹩\bar{M}\lt 0.1﹩ (orange), and ﹩\bar{M}\lt 0.08﹩ (green). Dotted lines indicate Gaussian-equivalent 2σ, 3σ, and 4σ thresholds. The dashed vertical lines indicate the values of the detection statistics for the unscrambled data set. We find little difference between the background distributions computed using different match thresholds, modulo the fact that imposing a smaller threshold yields fewer sky scrambles, which limits the precision to which the p-value can be measured.
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Top: MCOS HD S/N values recovered in the three simulations described in Appendix H.1, compared to the MCOS HD S/N measured in the real data set (vertical dashed red line), which has p-values of <10−2 for simulations (i) and (iii) and 0.64 for simulation (ii). Bottom: MCOS monopole S/N values recovered in the three simulations, compared to the real-data MCOS monopole S/N (vertical dashed red line), which has p-values of 4 × 10−2, 1.1 × 10−1, and <10−2 for simulations (i), (ii), and (iii), respectively.
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Distribution of real-data and replicated MCOS monopole S/Ns. Each point represents a draw  η  (k) from HD 13/3 posterior, which is used to simulate ﹩{\boldsymbol{\delta }}{{\boldsymbol{t}}}^{\left.{\rm{sim}},({\rm{k}}\right)}﹩ and to compute both S/Ns. The replicated monopole S/N is greater for 11% of the simulations.
Paper: Evidence for Ubiquitous Carbon Grain Destruction in Hot Protostellar Envelopes
Authors: Pooneh Nazari, Benoît Tabone, Merel L. R. van 't Hoff, Jes K. Jørgensen, Ewine F. van Dishoeck
Figure caption: Left panel is the same as Figure 2 but with the addition of C2H3CN (orange squares) and HNCO (green circles). For C2H3CN, given the data points are only approximate with no error bars, the non-weighted mean and standard deviation are shown. For all molecules, the upper limits are eliminated before calculating the (weighted) mean and standard deviation. The warm components of HNCO and C2H3CN are taken from Nazari et al. (2022b). The right panel presents the weighted (by the errors) mean of log10 of the ratios of hot to warm number of molecules with the weighted standard deviation of log10 of the data points for each molecule as the error bars. The hot to warm ratios of molecules without oxygen are at least ∼0.7 dex higher than those with oxygen.
Paper: Evidence for Ubiquitous Carbon Grain Destruction in Hot Protostellar Envelopes
Authors: Pooneh Nazari, Benoît Tabone, Merel L. R. van 't Hoff, Jes K. Jørgensen, Ewine F. van Dishoeck
Figure caption: The approximate temperatures at which various components from dust grains enter the gas in the envelope around a young star. At temperatures below ∼100 K (cold) all complex organic molecules (COMs) are in the ices. At temperatures above ∼100 K (warm) many COMs including CH3CN and CH3OH sublimate into the gas. At temperatures of around 400 K (hot) aromatic compounds evaporate (Gail & Trieloff 2017), and at similar temperatures refractory organics are thought to enter the gas through sublimation or pyrolysis (Nakano et al. 2003; Gail & Trieloff 2017; Li et al. 2021). Finally, at temperatures of ∼1000 K (very hot) pure amorphous carbon grains are thought to get destroyed through oxidation (Finocchi et al. 1997; Lee et al. 2010; Gail & Trieloff 2017) or UV photolysis (Alata et al. 2014; Anderson et al. 2017; Klarmann et al. 2018). The physical scale of each region is shown for a typical high-mass protostellar system.
Paper: Evidence for Ubiquitous Carbon Grain Destruction in Hot Protostellar Envelopes
Authors: Pooneh Nazari, Benoît Tabone, Merel L. R. van 't Hoff, Jes K. Jørgensen, Ewine F. van Dishoeck
Figure caption: Ratios of hot to warm number of methanol (blue circles) and methyl cyanide (red squares) molecules for the sources considered in this work. The dashed red and blue lines indicate the weighted mean (by errors) of log10 of methyl cyanide and methanol data points. The shaded regions show the respective weighted standard deviation (by errors) of log10 of the ratios around the mean. The values for the warm components are taken from Nazari et al. (2022b) for these sources and are calculated from the 13C and 18O column densities of methyl cyanide and methanol, respectively. There is an enhancement of a factor ∼4–5 in the hot component of methyl cyanide compared to methanol.