adsabs/AstroCLIMB huggingface dataset:
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: The spectral energy distribution (SED) of HD 136164 A. Archival photometry is overplotted a BT-NextGen model spectrum with T eff = 8100 K and ﹩\mathrm{log}(g)=4.2﹩. This spectrum is used to transform the companion’s contrast spectra into flux calibrated spectra.
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: The 3.3 mm dust continuum image (left top) and the velocity-integrated intensity maps of the molecular line emission (others) in the V883 Ori disk. The velocity range for integration is ±3.5 km s−1 with respect to the source systemic velocity v sys = 4.25 km s−1 (Tobin et al. 2023) including CH3OCH3 and CH3COCH3, where multiple blended transitions are integrated together. The molecular species, transitions, and upper state energy levels are indicated in the upper left corner of each panel. The black contours start from 5σ with steps of 2.5σ, where σ is the noise level of each map measured on the emission-free region, spanning σ = 1.8–4.4 mJy beam−1 km s−1 depending on the maps. The synthesized beam and a scale bar of 80 au are shown in the lower left and right corner of each panel, respectively.
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: Spectra corrected for Keplerian rotation toward the V883 Ori disk (gray). The model spectra for each species are shown in 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: Line plus continuum spectra of SPW 2 averaged over 1.″2 aperture for the CLEAN image (dark gray), the CLEAN model (gray), and the residual (light gray). The CLEAN model spectrum (in units of Jy pixel−1 by default) is scaled up by a ratio of the CLEAN beam area to the pixel area for visual clarity. The spectral line emission is almost fully recovered into the CLEAN model, and none of that remains in the residual spectrum. The horizontal dashed line indicates the zero-flux level.
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: Disk-integrated spectra toward V883 Ori without spectral alignment. The emission is integrated over the deprojected disk region with the outer radius of 0.″6 (or 240 au).
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: Continuation of Figure 19.
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: Disk-integrated spectra toward V883 Ori after the spectral alignment, overlaid with the best-fit model. The black solid lines indicate the full model composed of all detected species, while dashed colored lines are the model for each species shown in the legend. The gray-shaded region is removed from the fit (see Section 3.3 for details.)
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: Continuation of Figure 15.
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: Continuation of Figure 14.
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: Continuation of Figure 18.
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: Continuation of Figure 13.
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: Continuation of Figure 17.
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) High-resolution ALMA map of G203.21-11.20W2 in SiO emission integrated from −50 to +50 km s−1 with sensitivity σ = 4.6 K km s−1. The CO contours are overplotted from Figure 4(a). The synthesized beam size ∼0.″41 × 0.″34 is shown in the lower left corner. The jet axis is shown with a yellow dashed line, i.e., peak of the 1.3 mm continuum adopted from Dutta et al. (2020). (b) PV diagram along the jet axis of SiO emission with sensitivity σ = 0.15 K km s−1. The CO contours are the same as in Figure 4(b). The beam sizes are shown in the lower left corner (in red). The dashed lines at velocity = 33 km s−1 are the mean jet velocity, V  j  (uncorrected for inclination). The knot location is marked in B1, B2, ..... and R1, R2, .... in blue- and redshifted lobes, respectively. The “?” mark indicates that the knot positions could not be confirmed from the present observations. The magenta cross in each panel denotes the location of the continuum peak.
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) High-resolution ALMA map of G203.21-11.20W2 in CO emission integrated from −50 to +50 km s−1. The contours are overplotted at 3 × (1, 2, 3, 4, 6, 8, 12)σ, where sensitivity σ = 4.8 K km s−1. The synthesized beam size ∼0.″41 × 0.″34 is shown in the lower left corner. CO emission is extended in the northwest-to-southeast direction with a position angle of ∼122°. The cyan (blueshifted) and red (redshifted) parabolas are best fits assuming a proportionality constant c = 0.5 arcsec−1. (b) PV diagram along the jet axis of 12CO (2−1) emission. The black contours are at 3 × (1, 2, 3, 4, 5, 6)σ, where sensitivity σ = 0.11 K. The beam sizes are shown in the lower left (in red) emission. The red and cyan parabolas here are for inclination angle, i = 20°. Cyan and red represent the northwest and southeast direction, respectively, in panel (a). The magenta cross in each panel is the location of the continuum peak.
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: high-resolution C18O map of G203.21-11.20W2 integrated over +8−12 km s−1. The sensitivity is 15 mJy beam−1 km s−1. The red contours are high-resolution continuum contours at (3, 6, 12, 24, 36) × σ, where the sensitivity σ = 0.04 mJy beam−1, adopted from Dutta et al. (2020). The black contours are the same as in Figure 1. The beam sizes are shown in order of C18O, high-resolution continuum, and ACA resolution continuum. The jet axis is also shown (brown dashed line). Right: the C18O spectrum of G203.21-11.20W2 extracted from high-resolution maps from the box region in the left panel. The vertical line indicates the systemic velocity of the object determined from the spectrum at V sys = 10 km s−1.
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: Example image of ALMA 1.3 mm continuum emission detected toward protostar G203.21-11.20W2. The typical beam size of ∼7.″52 × 5.″52 (80.°7) is shown in red in the lower left corner. The contours are at 3 × (1, 2, 4, 8, 12)σ, where the sensitivity σ = 0.4 mJy beam−1. The cross indicates the continuum center at high resolution, adopted from Dutta et al. (2020). The blue dashed line indicates the outflow/jet axis, determined from the SiO emission. A scale bar is also shown for context.
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: Histogram of envelope masses estimated using 1.3 mm emission at a resolution of ∼7.″6 × 4.″1.
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: G212.84-19.45N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.5 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 = 4 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 1.24 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.12 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: G211.01-19.54S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.4 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 = 6 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 2.21 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.13 K, with similar symbols and contours to those in Figure 4(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: G192.32-11.88S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼3.5 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) Integrated CO emission with sensitivity 6.6 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G211.01-19.54N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼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 = 6 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 6.3 K km s−1, with similar symbols and contours 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).
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: G208.68-19.20S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼10 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) Integrated CO emission with sensitivity 1.5 K km s−1, with similar symbols and contours 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).
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: G206.93-16.61E2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.5 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) Integrated CO emission with sensitivity 37.5 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G205.46-14.56N1. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.5 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) Integrated CO emission with sensitivity 9.2 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G205.46-14.56S2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.7 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) Integrated CO emission with sensitivity 6.0 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G201.52-11.08. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.5 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) Integrated CO emission with sensitivity 1.4 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G215.87-17.62N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.7 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 = 10.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 5.21 K km s−1, with similar symbols to those in Figure 4(a).
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: G207.36-19.82N1. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.5 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) Integrated CO emission with sensitivity 6.13 K km s−1, with similar symbols and contours to those in Figure 4(a).
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: G212.10-19.15N2. (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 = 4.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 2.14 K km s−1, with similar symbols to those in Figure 4(a).
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: G210.97-19.33S2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.7 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 = 3.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 8.0 K km s−1, with similar symbols to those in Figure 4(a).