adsabs/AstroCLIMB huggingface dataset:
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Reconstructed radial intensity profiles of CH3OH (blue), CH3CHO (orange), and CH3OCHO (green) transitions. The horizontal gray dashed line indicates the zero-intensity level. The gray dashed curve shows the radial intensity profile of CH3OH transition in Band 6 created by deprojection and azimuthal averaging on the higher-resolution (∼0.″1) velocity-integrated intensity maps (Tobin et al. 2023). The Band 6 intensity profile is normalized by its radial peak being matched to the radial peak of the Band 3 CH3OH profile.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Kernel density estimate of the posterior probability density distributions of column density ratios of 12C- to 13C isotopologues for CH3CHO, CH3OCHO, and CH3OCH3. Two isomers of 13C isotopologues are observed for CH3CHO and CH3OCHO. The probability density is normalized by the peak being unity and offset for visual clarity. The ISM value of 69 is marked by the vertical dashed line. We note that the 12C/13C ratios of CH3CHO and CH3OCH3 are based on the tentatively detected transitions of 13C isotopologues, and therefore should be considered as lower limits.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Line profiles of CH3OH 2−1,1–1−1,0 E v  t  = 0, CH3CHO 52,3–42,2 E v  t  = 0, and CH3OCHO 76,1–66,0 E v  t  = 0. The vertical gray dotted line marks the systemic velocity (4.25 km s−1). The vertical blue dashed lines indicate the corresponding disk radii at each velocity channel based on the maximum velocity of Keplerian rotation in Equation (1). The horizontal gray dashed line indicates the zero-flux level. There are no significant emission at the velocity channels, which corresponds to inside ∼40 au radius.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Channel maps of the CH3OH 2−1,1–1−1,0 E v  t  = 0 transition. The black contours mark the [−3, 3, 5, 7, ...]  ×  σ levels. The dashed contours indicate the negative values. The numbers in the upper right and upper left corners indicate the velocity of the channel and its corresponding Keplerian radius (﹩r={{GM}}_{\star }{\sin }^{2}i/{(v-{v}_{\mathrm{sys}})}^{2}﹩), respectively. The red cross in each panel indicates the position of the disk center. The beam is shown in the lower left corner of the lower left panel.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Comparison of the COM D/H ratios in the V883 Ori disk with those in IRAS 16293 B (Jørgensen et al. 2018) and 67P/C-G (Drozdovskaya et al. 2021) from literature. The different colors indicate the different molecular species of COMs as shown in the legend. Upper limits are shown by the downside arrows. The CH2DOH/CH3OH ratio in V883 Ori is shown by a semitransparent circle to indicate its large uncertainty due to the large uncertainty in the spectroscopic data of CH2DOH.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Demonstration of the simultaneous spectral fit for a selected frequency range in SPW 7. The observed spectra (gray) is well reproduced by the model (black) composed of multiple blended transitions of different species, CH3OH, CH3CHO, CH3COCH3, c-C2H4O, and CH﹩{}_{3}^{13}﹩CHO (dashed colored lines).
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Same as Figure 9, but for CH3OCHO 85,3–75,2 A v  t  = 0 transition.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Same as Figure 9, but for CH3CHO 52,3–42,2 E v  t  = 0 transition.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: Left: a zoomed-in view of the jet of G191.90-11.21S compared with a schematic diagram. Middle: the SiO integrated map (same as in Figure 6). CO emission is integrated over −4 to +8 km s−1 with sensitivity σ ∼ 6.48 K km s−1 with contour levels at (24, 27, 30, 33, 36) × σ. The location of the central core is at (0, 0). The left panel is the SiO PV diagram with sensitivity 0.16 K, and CO contours are overplotted at 3 ×  (1, 2, 3, 4, 5, 6)σ in red. More details on SiO and CO images are included in Appendix B.1 and Figure B1. Right: the schematic diagram based on observations that illustrate general morphologies of the 1.3 mm continuum and the C18O, CO, and SiO line emission. The 1.3 mm continuum and C18O emission trace the disk and envelope (comparing with Figure 3(a)). CO emission delineates the outflow shell and whole knot structure, including a CO emission forward front, a SiO+CO emission middle shock front, and a CO emission backward front.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: A schematic diagram illustrating a mechanism whereby a bipolar jet can appear to be a monopolar jet. (a) Each knot consists of three observed layers: a forward CO emission front (in red), a middle SiO+CO front (in green), and a backward CO emission front (in blue). (b) Close-up view of a knot in the redshifted lobe. The colors are the same as in panel (a). An additional compressed layer is highlighted between the forward CO front and middle SiO+CO front. (c) The possible temperature distribution of the knot of panel (b) is plotted, following the simulation results by Lee et al. (2001). Layers iii and iv have the highest temperature, and layer i is cooler than layers iii and iv. Layer ii, however, exhibits a temperature discontinuity or is much cooler than the other layers. The density of layer ii is greater than that of the other layers. For the redshifted lobe, an observer can see the middle SiO+CO (layer iii) and backward CO layers (layer iv). For the blueshifted lobe, the scenario is opposite, where an observer can see only a forward CO emission front (layer i). Emission from layers iii and iv might be shielded by the compressed and coolest layer ii. In that case, only the CO jet can be observed in blueshifted emission. If layer i is not dense enough, then even CO emission in the blueshifted lobe of the jet cannot be detected.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: SiO-to-CO abundance ratios, X SiO/X CO = N SiO/N CO, are plotted as a function of observed jet mass-loss rate (﹩{\dot{M}}_{j}﹩ or ﹩{\dot{M}}_{\mathrm{obs}}﹩). The error bars in the abundance ratios represent the lower limit since SiO is optically thicker than CO. The abundance ratios of HH 212 (in red) and HH 211 (in blue) are calculated from the column densities in the published literature (HH 212, Lee et al. 2007a; HH 211, Jhan & Lee 2021). Asymptotic abundance ratios (gray lines) are adopted from Tabone et al. (2020), estimated using the Paris–Durham shock code designed to model irradiated environments and a laminar 1D disk wind model. The model considered a streamline launched at R 0 = 0.15 au with T = 1000 K in the disk for dust-free models (dust-to-gas mass ratio Q = 0) and dust-poor models (Q = 6×10−6, 6×10−5, and 6 × 10−4), as well as for different values of wind mass-loss rates (﹩{\dot{M}}_{w}﹩) referring to theoretical models that account for the origin of jets. The shaded region indicates the location of most of the observed data.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: High-resolution integrated over whole SiO emission velocity range of monopolar or likely monopolar SiO jets of protostars. The contours and symbols are the same as in Figure 5(a). The SiO and CO velocity information and sensitivity are added in the associated figures in the appendices.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: SiO emission along the outflow/jet axis. The SiO emission is not well characterized as jet emission in this study. All the symbols are the same as in Figure 6. Faint SiO emission locations are marked in some of the panels. The “??” mark for T bol and L bol indicates that these values are yet to be determined and not available in the literature. The “?” mark indicates that the structures could not be confirmed from the present observations.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: (a) Jet velocities (V  j ) are plotted as a function of (a) bolometric luminositiy (L bol) and (b) envelope mass (M Env) estimated from ACA continuum. The color bar indicates the ratio of mass ejection rate to accretion rate (﹩{\dot{M}}_{j}﹩/﹩{\dot{M}}_{\mathrm{acc}}﹩), where the mass accretion rates ﹩{\dot{M}}_{\mathrm{acc}}﹩ were estimated for a protostellar mass of 0.1 M ⊙ and total luminosity using Equation (6). Objects with increasing trends are marked with an ellipse to guide the eye. A linear fit of the data points is shown in panel (b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: Inclination-corrected mean jet velocities V  j,cor = ﹩\tfrac{{V}_{j}}{\sin i}﹩ are shown as a function of ﹩\sin i﹩, where i is the measured inclination angle. The mean value of V  j,cor  =  112 km s−1 is also shown. Monopolar and bipolar jets are shown as circles and squares, respectively.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: Bipolar jets in SiO emission. All the symbols are the same as in Figure 6. The “??” mark for T bol and L bol indicates that these values are yet to be determined and not available in the literature.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G210.49-19.79W (HOPS 168). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 7 km s−1. All symbols are the same as in Figure 3. (c) CO emission map integrated over −45 to +55 km s−1 with sensitivity 6.0 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.15 K, with similar symbols and contours to those in Figure 4(b). The additional likely episodic shells are marked with thick blue and red lines in the blueshifted and redshifted lones, respectively. (e) SiO map integrated over −20 to +20 km s−1 with sensitivity 1.9 K km s−1, with similar symbols and contours to those in Figure 5(a). The knots shifted from jet axis are marked. (f) SiO PV diagram with sensitivity σ = 0.15 K, with similar symbols to those in Figure 5(b). The “?” mark indicates that the present observations could not confirm the scenario.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G208.89−20.04E. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.2 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 9 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −4 and +2−6 km s−1 with sensitivity σ ∼ 1.52 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −4 to +4 km s−1 with sensitivity 1.7 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.32 K, with similar symbols and contours to those in Figure 5(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G209.55-19.68S1 (HOPS 11). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 8 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −8 to −4 km s−1 and +4−8 km s−1 with sensitivity σ ∼ 6.6 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −60 to +60 km s−1 with sensitivity 8.0 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.15 K, with similar symbols and contours to those in Figure 5(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G215.87-17.62M. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −10 to −4 km s−1 and +2−10 km s−1 with sensitivity σ ∼ 5.8 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.21 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −40 to +38 km s−1 with sensitivity 2.5 K km s−1, with similar symbols and contours to those in Figure 4(a). (f) SiO emission with sensitivity 0.13 K, with similar symbols and contours to those in Figure 4(b). The “?” mark indicates that the present observations could not confirm the scenario.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G209.55-19.68S2 (HOPS 10). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 8 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −4 to −2 km s−1 and +2−4 km s−1 with sensitivity σ ∼ 5.8 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.21 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over +40−58 km s−1 with sensitivity 2.5 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.21 K, with similar symbols and contours to those in Figure 5(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G208.68-19.20N3. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼10.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 12 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −12 to +12 km s−1 with sensitivity σ ∼ 9.65 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission inetgrated over −66 to +58 km s−1 with sensitivity 4.6 K km s−1, with similar symbols and contours to those in Figure 5. (f) SiO PV diagram with sensitivity 0.15 K, with similar symbols and contours to those in Figure 5(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G210.37-19.53S (HOPS 164). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 8 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −6 to −2 km s−1 and 0−4 km s−1 with sensitivity σ ∼ 5.8 K km s−1, with similar symbols to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.21 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −46 to −24 km s−1 and +30−48 km s−1 with sensitivity 2.5 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.21 K, with similar symbols and contours to those in Figure 5(b).