adsabs/AstroCLIMB huggingface dataset:
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Left: JWST/NIRCam image of HH 46/47, taken from the Mikulski Archive for Space Telescopes (MAST), obtained as part of the DDT program PID4441 (P.I. K. Pontoppidan). The image combines the F200W and F335M filters, which primarily trace the H2 emission, while the F115W filter was used as a jet tracer. Right: enlargement of the region observed by PROJECT-J. The H2 emission from the red- and blueshifted lobes is shown in magenta and cyan, respectively. The [Fe II] 5.5 μm emission tracing the red- and blueshifted atomic jet is overlaid in red and blue, respectively. The black star marks the source position. The main structures identified in Paper I—such as the atomic jet, molecular cavity, compact knots, and bow shocks—are labeled for reference.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: Location of 46 HADS stars in the H-R diagram in this work (red squares), along with 35 well-studied HADS (blue dots) collected from D. H. McNamara (2000), E. Poretti et al. (2005, 2011), J. L. Christiansen et al. (2007), L. A. Balona et al. (2012), C. Ulusoy et al. (2013), J. H. Peña et al. (2016), T. Yang et al. (2018), T.-Z. Yang & A. Esamdin (2019), D. M. Bowman et al. (2021), and T.-Z. Yang et al. (2021b). The ZAMS and the δ Sct instability strip (solid lines) are from S. J. Murphy et al. (2019). The yellow dotted–dashed lines represent the boundaries of the instability strip predicted by D. R. Xiong et al. (2016). The dashed lines show the region occupied by HADS, as found by D. H. McNamara (2000). The theoretical instability strip (IS) of γ Dor stars (black dotted–dashed lines), as well as the calculated positions of the blue and red edges for the fundamental mode (green dotted–dashed lines), are from M. A. Dupret et al. (2005).
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: JWST/NIRSpec stacked H2 line intensity map, obtained by combining the v = 1–0 rovibrational transitions from S(1)–S(3) and O(2)–O(7). White contours delineate the brightest regions of the stacked H2 emission (levels from 0.085 to 2.0 MJy sr−1), highlighting the arc-shaped morphology of knot A1. Cyan contours trace the [Fe II] 1.81 μm emission (levels from 0.028 to 0.4 MJy sr−1), outlining the collimated jet. The two components of the binary system are marked with stars: the white star denotes the primary source (a⋆), and the yellow star marks the secondary (b⋆). Blue and yellow lines indicate the newly identified A3b and A1b arcs, associated with the jet from a⋆ and the outflow from b⋆, respectively.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: Continuum-subtracted map of the H2 0–0 S(4) line at 8.03 μm. The NIRSpec FOV is outlined by a black square. Representative regions within the outflow, selected for further analysis, are indicated with white circles. Each circular aperture has a radius of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4.
Paper: PROJECT-J: The Shocking H2 Outflow from HH 46
Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, Jochen Eislöffel, Patrick Hartigan, Alberto Noriega- Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan
Figure caption: MIRI continuum-subtracted H2 line intensity maps of pure rotational transitions. White stars mark the positions of the two sources. Contours of the 0–0 S(7) line at 5.51 μm (levels from 0.6 to 10.0 MJy sr−1) are overlaid on the 0–0 S(1) map at 17.04 μm. The contours clearly show that the MIRI FOV varies with wavelength, ranging from 6″ × 15″ for the 0–0 S(8) line at 5.05 μm to 8″ × 17″ for the 0–0 S(1) line at 17.04 μm.
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: PL relation of the 46 HADS stars in this work. The blue solid line is the PL relation of HADS stars derived by D. H. McNamara (2011), the green solid line is from E. Ziaali et al. (2019), the black dashed line is from T. Jayasinghe et al. (2020), and the red solid line (for the fundamental mode) and red dotted–dashed line (for the first overtone mode) are from A. Poro et al. (2021).
Paper: Pulsation Mode Identification and Classification of 46 High-amplitude δ Scuti Stars from 50 Candidates with TESS Observations
Authors: Taozhi Yang, Zhaoyu Zuo
Figure caption: The upper panel shows a portion of the light curve of TIC 36736263 for about 3 days. The middle panel shows the phase diagram folded by the only detected frequency, f = 13.69986 c day−1. The lower panel shows the Fourier amplitude spectra.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Stellar cycle variability as obtained from three different dynamo models as a function of the Rossby number (dashed line and bottom x-axis) and ﹩{\mathrm{log}}\,{({P}_{{\rm{cyc}}}/{P}_{{\rm{rot}}})}^{2}﹩ (solid line and top x-axis). Models and the variability definition are the same as in Figure 6.
Paper: Stellar Cycle Variability in Mount Wilson Stars and Dynamo Models: Rotation Rate and Dynamo Number Dependency
Authors: Suyog Garg, Rohan B. Mandrai, Bidya Binay Karak
Figure caption: Stellar cycle variability as obtained from three different dynamo models as a function of the stellar rotation period. The dynamo models are discussed in detail in Section 3, while the variability is defined in Equation (3).
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: nAGN and ﹩{n}_{{\rm{AGN}}}^{{\rm{eff}}}﹩ as a function of redshift. The black data points represent the total nAGN sampled by our data (λEdd > 0.0013). The red, yellow, and blue data points represent nAGN for AGNs accreting at λEdd = 0.01–0.1, λEdd = 0.1–1, and λEdd = 1–100, respectively. The black solid line represents ﹩{n}_{{\rm{AGN}}}^{{\rm{eff}}}﹩, and the dashed line represents nAGN for AGNs within the 25%–75% quantile range of 〈λEdd〉. The error bars of the data points and the gray shaded region for ﹩{n}_{{\rm{AGN}}}^{{\rm{eff}}}﹩ represent the 90% confidence intervals derived with our Monte Carlo method. For comparison, we show the total nAGN for AGNs with ﹩{\rm{log}}[{L}_{{\rm{X}}}/{\rm{erg}}\,{{\rm{s}}}^{-1}]\gt 42﹩ from J. Buchner et al. (2015; gray hatched region representing 10%–90% confidence intervals), T. Miyaji et al. (2015; green dotted line), and A. Peca et al. (2023; brown dotted–dashed line).
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: Top panel: ρBHAR as a function of redshift. The black data points represent the total ρBHAR sampled by our data. The red, yellow, and blue data points represent ρBHAR for AGNs accreting at λEdd = 0.01–0.1, λEdd = 0.1–1, and λEdd = 1–100, respectively. For comparison, the cosmic SFRD (P. Madau & M. Dickinson 2014) scaled by a factor of 5000 is shown as the dashed line to approximate the peak of ρBHAR at z ≈ 2. The green dotted line and the brown dashed line represent the total ρBHAR from Y. Ueda et al. (2014) and G. Yang et al. (2018), respectively. Bottom panel: logarithm of the ratio of ρBHAR contributed by AGNs with λEdd > 0.1 to that contributed by AGNs with λEdd < 0.1. The error bars represent the 90% confidence intervals derived with our Monte Carlo method.
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: The evolution of 〈λEdd〉 and 〈MBH〉 at different redshifts, with colors defined in the legend. Top panel: the error bars show the region bounded by the 25%–75% quantiles of ﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩ and ﹩\mathrm{log}\langle {M}_{{\rm{BH}}}\rangle ﹩ in Figure 3, assuming the median p(λEdd∣M⋆, z) and MBH = 0.002M⋆. Bottom panel: the error bars represent the 90% confidence intervals derived with our Monte Carlo method. From z = 1.5–2.0 to z = 0.2–0.5, 〈λEdd〉 and 〈MBH〉 both decrease; 〈λEdd〉 decreases by 1.35 dex, but 〈MBH〉 decreases by only 0.21 dex.
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: Contribution to ρBHAR per galaxy at different redshifts assuming the median p(λEdd∣M⋆, z) and MBH = 0.002M⋆. The color bars represent the logarithm of (1 − ϵ)/(ϵc2) × F(λEdd, M⋆∣z) × M⋆λEddκ(M⋆). The median values of ﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩ (﹩\mathrm{log}{M}_{{\rm{BH}}}﹩) at fixed ﹩\mathrm{log}{M}_{{\rm{BH}}}﹩ (﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩) are shown as solid (dashed–dotted) curves. The 25%–75% quantiles of ﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩ (﹩\mathrm{log}{M}_{{\rm{BH}}}﹩) at fixed ﹩\mathrm{log}{M}_{{\rm{BH}}}﹩ (﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩) are shown as dotted (dashed) curves. The error bars represent the ﹩\mathrm{log}\langle {\lambda }_{{\rm{Edd}}}\rangle ﹩ and ﹩\mathrm{log}\langle {M}_{{\rm{BH}}}\rangle ﹩ that roughly span the region enclosed by the 25%–75% quantiles of ﹩\mathrm{log}{\lambda }_{{\rm{Edd}}}﹩ and ﹩\mathrm{log}{M}_{{\rm{BH}}}﹩.
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: AGN host-galaxy SMF ﹩{\phi }_{{\rm{M}}}^{{\rm{AGN}}}﹩ at different redshifts, with colors defined in the legend. The left, middle, and right panels show the λEdd = 0.01–0.1, λEdd = 0.1–1, and λEdd = 1–100 bins, respectively. For comparison, the galaxy SMF at z = 0.2–0.5 of J. R. Weaver et al. (2023) is shown as black solid curves. The colored shaded stripes represent the 1σ uncertainty from p(λEdd∣M⋆, z).
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: Top panels: ﹩\overline{{L}_{{\rm{bol}}}^{{\rm{AGN}}}}﹩ (left) and fAGN (right) as functions of redshift at different M⋆, with colors defined in the legend. Bottom panel: the decline in ﹩\overline{{\rm{BHAR}}}﹩ (gray solid), ﹩\overline{{L}_{{\rm{bol}}}^{{\rm{AGN}}}}﹩ (blue dashed), and fAGN (red dashed–dotted) from ﹩{\rm{log}}({M}_{\star }/{M}_{\odot })=11.5﹩ to ﹩{\rm{log}}({M}_{\star }/{M}_{\odot })=10﹩ as functions of redshift. The colored shaded stripes represent the 1σ uncertainty from p(λEdd∣M⋆, z).
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Schematic of collision simulations of pebbles. We generate a BCCA and compress it in three dimensions using periodic boundaries. We extract a spherical region from the compressed BCCA for the fiducial cases. For larger aggregates, we combine eight compressed BCCAs before carving out a spherical region. We suppress the monomer oscillations and remove isolated monomers. We let two identical aggregates collide with random relative orientations. After the collision at a velocity of v0, contact points are determined as the midpoints of two contacting monomers from different pebbles.
Paper: The Drivers of the Decline in Supermassive Black Hole Growth at z < 2
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Bin Luo, Qingling Ni, D. P. Schneider, Fabio Vito
Figure caption: Comparison of ρBHAR (left panel) and nAGN (right panel) for results excluding eFEDS (data points with error bars) and including eFEDS (shaded regions). Error bars and shaded regions indicate 90% statistical uncertainties, with colors matching those in the legend of the left panel.
Paper: Mid-infrared Extinction toward the Galactic Center
Authors: Sebastiano D. von Fellenberg, Joseph M. Michail, S. P. Willner, Braden Seefeldt-Gail, Tamojeet Roychowdhury, Macarena Garcia Marin, Giovanni G. Fazio, Nicole M. Ford, Daryl Haggard, Joseph L. Hora, Howard A. Smith, Zach Sumners, Gunther Witzel
Figure caption: Best overall MIR extinction law. The blue curve shows the continuum extinction shifted by −0.18 ± 0.02 mag to match the line-derived extinction values (filled brown and orange points). The continuum model is the average of the Sgr A* and Mini-spiral model. The fit excludes the four lines most affected by residual fringing: 5.957, 6.292, 6.772, and 11.309 μm, indicated by open points. The gray dashed line shows the extinction law derived by T. K. Fritz et al. (2011), and gray points show the stellar-color-based extinction law by R. Schödel et al. (2010). The relative extinction measurements were calibrated using A7.46 = 0.64 mag. Violin plots show the spread of values using the pixel-by-pixel extinction measurements; the brown and orange points show the measurements for two apertures centered on Sgr A* and the Mini-spiral shown in Figure 7. The data behind this figure, including the median posterior model and posterior samples, are available.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Mid-infrared Extinction toward the Galactic Center
Authors: Sebastiano D. von Fellenberg, Joseph M. Michail, S. P. Willner, Braden Seefeldt-Gail, Tamojeet Roychowdhury, Macarena Garcia Marin, Giovanni G. Fazio, Nicole M. Ford, Daryl Haggard, Joseph L. Hora, Howard A. Smith, Zach Sumners, Gunther Witzel
Figure caption: Spatial variation of the line-derived extinction values for the 5.129 μm and 5.908 μm hydrogen recombination lines. The color bar shows the relative extinction measurements from the line ratios (A5.129/7.46 and A5.908/7.46) after they were converted to absolute extinction values by adding A7.46 = 0.64 mag derived from the Mini-spiral extinction measurement (Section 4.2). The white cross shows the approximate location of Sgr A*, and the lighter patches illustrate the two aperture masks used to obtain the line measurements in Figure 7. The rightmost panel shows the K-band extinction map derived from stellar colors (R. Schödel et al. 2010). The K band has higher absolute extinction (﹩{\left\langle A\right\rangle }_{2.16}\approx 2.4\,{\rm{mag}}﹩) but shows spatial variations similar to the MIR.
Paper: Mid-infrared Extinction toward the Galactic Center
Authors: Sebastiano D. von Fellenberg, Joseph M. Michail, S. P. Willner, Braden Seefeldt-Gail, Tamojeet Roychowdhury, Macarena Garcia Marin, Giovanni G. Fazio, Nicole M. Ford, Daryl Haggard, Joseph L. Hora, Howard A. Smith, Zach Sumners, Gunther Witzel
Figure caption: Spatial variation of the line-derived extinction values for all lines with S/N > 6. Pixels with S/N < 6 are flagged. As in Figure 8, the white cross marks the Sgr A* position, and the lighter or gray patches indicate the two aperture areas where the lines were measured. Residual fringing may have affected the spatial correlation. (See text for details.) The color maps have different minima and maxima, but have been scaled to illustrate the spatial variations in the field. The white crosses mark the approximate location of Sgr A*.
Paper: Mid-infrared Extinction toward the Galactic Center
Authors: Sebastiano D. von Fellenberg, Joseph M. Michail, S. P. Willner, Braden Seefeldt-Gail, Tamojeet Roychowdhury, Macarena Garcia Marin, Giovanni G. Fazio, Nicole M. Ford, Daryl Haggard, Joseph L. Hora, Howard A. Smith, Zach Sumners, Gunther Witzel
Figure caption: Extinction correction applied to a bright state of Sgr A*. The top panel shows a power-law fit to the differential flux measurements, and the bottom panel shows the deviations from a power law. The blue areas indicate the extinction uncertainty derived from the dust continuum modeling. The data were first presented by S. D. von Fellenberg et al. (2025), and J. Michail et al. (2025) gave a detailed analysis of the spectrum.
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: The spin angular momenta of clumps, both transient and persistent, identified in runs C, D, D-Zoom-P, D-Zoom-O, B-hiZ, and C-hiZ, in Hill units (top) and scaled by Jcrit (bottom; Equation (16)). Also shown are the orbital angular momenta of observed CCKB binaries with measured inclinations ibin (defined as the angle between the binary orbit normal and the heliocentric orbit normal; data from D. Nesvorný et al. 2021). Data for clumps are color-coded by obliquities; ibin for observed CCKB binaries uses the same color scale. For observed binaries, Rplan is the mean radius of the binary components (data from W. R. Johnston 2019). For simulated clumps, Rplan is computed as the radius of a single planetesimal of material density ρ• = 1 g/cc, assuming a given clump forms two such planetesimals in an equal-mass binary. All simulation-based data in this figure are evaluated at the onset of a clump’s formation, when clump properties are best compared to the predicted value (Equation (19)) from the SI (by contrast, Table 1 evaluates Rplan at either the end of the simulation for a bound clump or just before dispersal for a transient clump). The simulated clumps show systematically higher J than observed binaries; this discrepancy is expected to lessen as the clumps lose angular momentum during their collapse (see Section 3.2.1 and D. Nesvorný et al. 2021).
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Similar to Figure 1 but for turbulent gas bump simulations (Table 2). The third panel from the top shows the Gaussian-fitted radial width of the dust ring. Only run Bu-100 forms planetesimals, but the formation efficiency (from wholesale gravitational collapse) is too large, resulting in a planetesimal belt nearly 2 orders of magnitude more massive than the CCKB today (bottom panel).
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Snapshots of particle surface density (top row) and azimuthally averaged volume density (bottom row) for turbulent gas bump simulations (runs Bu) at ﹩t=100{{\rm{\Omega }}}_{0}^{-1}﹩ (﹩80{{\rm{\Omega }}}_{0}^{-1}﹩ for run Bu-100). Either no planetesimals form (left and middle columns) or too many form (right), with no middle ground to match the present-day properties of the CCKB. For quantitative details, see Figure 9 and Table 2. Simulation videos are available at rixinli.com/CCKB.
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Same as Figure 2 but showing snapshot sequences from run C-hiZ, which yields two surviving clumps at x(Hg) ≈ −0.6 to −0.7. Simulation videos are available at rixinli.com/CCKB.
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Comparison of the obliquity distributions of clumps (both transient and persistent) collected from runs C, D, B-hiZ, C-hiZ, D-Zoom-P, and D-Zoom-O and the inclination distribution of observed CCKB binaries (gray dashed line; W. Grundy et al. 2019). The simulated obliquity distributions in the four standard-resolution runs are uncertain as they each rely on just a handful of clumps (two to seven, depending on the run). The zoomed-in runs resolve 60–68 clumps having obliquities more closely resembling CCKB binary inclinations.
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Comparison of snapshots of particle surface density (top row) and azimuthally averaged volume density (bottom row) between the original run D (Δx = H/1040) and the zoomed-in simulation run D-Zoom-P (Δx = H/2560) at ﹩t=70{{\rm{\Omega }}}_{0}^{-1}﹩. While the large-scale morphology of the dust filament and background particle layer are similar between the two runs, many more self-gravitating clumps are evident in the higher-resolution simulation. Clumps are marked in the top row by white circles indicating Hill spheres.
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Same as Figure 1 but for the higher-metallicity runs with Z > 0.01 (height-integrated). See Table 1 for parameters.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: (a) PV diagram of C18O along the P.A. = 60° line passing through the position of the central source. White contour denotes the 5σ level. Blue and red points with error bars are the measured rotational velocities of the NE side (blueshifted) and the SW side (redshifted), respectively. Horizontal and vertical dashed lines are the position of the central source and the systemic velocity, respectively. The horizontal and vertical error bars in the bottom-left corner denote the velocity resolution of the data cube and the beam dimension along the position angle of the PV slice. (b) Log–log plot of the measured rotational velocity as a function of the projected radius. Blue and orange dots with error bars are the intensity-weighted positions at given velocities. Blue and orange crosses with error bars are the centroid velocities of the blue and red components, respectively, derived from the two-component Gaussian fitting.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: (a) Outflow shell model curve with C = 5.0 arcsec−1 (magenta curve) overlaid on the CO moment 0 map of the redshifted component. Contours are drawn every 5σ (1σ = 15 mJy beam−1 km s−1) with the lowest contour level at 10σ. (b) Model curve with C = 4.0 arcsec−1 (cyan curve) overlaid on the CO moment 0 of the blueshifted component. Contour stars from 10σ (1σ = 10 mJy beam−1 km s−1) with a step of 5σ. (c) and (d) PV diagrams along the axes of the redshifted lobe, P.A. = 0°. (c), and the blueshifted lobe, P.A. = −​​​​​​25°. (d). Blue and orange curves are the model curves produced by C = 5.0 arcsec−1 and i ∼ 40° for (c), and C = 4.0 arcsec−1 and i ∼ 40° for (d). The deflection point of the eastern wall of the southern lobe is indicated in panels (a) and (c).