adsabs/AstroCLIMB huggingface dataset:
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Histograms for the SDSS-V corrector design in the H band. (a) Spatial distribution, relative to the centroid location. (b) Angular distribution, relative to the focal surface normal.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: The final SDSS-V wide-field corrector design (thick design).
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: SESO AR coating design curves for the SDSS-V corrector. Plots are shown for 0° and 35° angle of incidence.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Encircled energy curves for the SDSS-V corrector design on a common focal surface. (a) Optical. (b) H band.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Spot diagrams for the SDSS-V corrector design on a common focal surface. (a) optical. (b) H band.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Rendering of the fixturing used to bond the SDSS-V lenses. The lens is supported initially by three Delrin stanchions on a rotary table. The cell is supported by three adjustable ball transfer supports to facilitate both centering and vertical adjustments. A Teflon sealing ring affixed to the bottom of the cell supports the lens once alignment is complete and seals the gap between the lens and cell during the bonding operation.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Rendered image showing the SDSS-V corrector L1/L2 assembly adjustment scheme.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Gravity-induced deflections for the three lenses of the SDSS-V corrector design: (a) Gravity vector aligned to the optical axis of the corrector, i.e., zenith pointing. (b) Gravity vector normal to the corrector optical axis, i.e., horizon pointing.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Distortion under gravity: (a) Contour plot showing residual distortion for zenith pointing. (b) Contour plot showing residual distortion for horizon pointing. Results are expressed in waves at 632.8 nm.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Rendered image of the SDSS-V corrector lens cell for L1.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Photograph of the SDSS-V corrector lens L2 after bonding.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Cross section showing the SDSS-V corrector optomechanical design.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Photograph of the SDSS-V corrector in the cleanroom at JHU just prior to shipment; the L3 assembly is in the foreground with the L1/L2 assembly directly behind it.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Section view of the SDSS-V corrector. Dimensions here are in inches, consistent with telescope mechanical units.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Logarithmically plotting the fill-out factors of CBs against their mass ratios. Small black circles and small red squares are the results of X.-Z. Li et al. (2024) for W- and A-type CBs, respectively. Blue squares show our joint-fitting results, and orange circles represent our results for systems on which we could only perform LC fitting.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Top left: retrieved median and maximum-likelihood P–T profiles, with 500 P–T profiles drawn from the posterior in black. Top right: maximum-likelihood emission contribution function, with observed orders shaded. Center: Fp/Fs for the maximum-likelihood and median retrieved planet models, compared with the expected Fp/Fs assuming the planet and star are blackbodies at their respective equilibrium and effective temperatures. Observed orders are shaded. Bottom: opacities of the species included in the retrieval over the observed bandpass.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Kp–Δvsys plots for the K-band (left), L-band (center), and combined (right) data sets using the maximum-likelihood retrieved planet model. HD 209458 b is weakly detected (SNR ≈ 4) in each band individually, improving to SNR ∼ 5 when both epochs are combined. The SNR is estimated by first median-subtracting each row of the Kp–Δvsys plots, then dividing by the standard deviation of the negative Kp region, which results in a slight offset of the maximum (indicated by a red dot) from the values in Table 2. See L. Finnerty et al. (2024, 2025a) for a more detailed discussion of the issues with estimating noise in Kp–Δvsys plots.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Kp–Δvsys plots for each molecule. Planet models were generated using the maximum-likelihood parameters, setting the specified mass fraction to 10−1.5 and all others to 10−15. Only H2O shows a clear peak consistent with the ephemeris of HD 209458 b. While CO, H2S, and HCN show SNR ∼ 3 peaks consistent with the planet, comparison to other molecules shows that features of comparable strength regularly appear at random locations in the Kp–Δvsys space. CO shows a strong peak at very negative Kp, which may be a result of stellar or telluric contamination.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: The upper panel displays a q = 0.066, l3 = 0.020 fit (magenta curve) overlaid on top of a q = 0.160, l3 = 0.510 synthetic LC (black points). The lower panel shows the residuals with a smoothed residual line (green line). The excellent agreement between the synthetic strong-l3 LC and the extreme-q fit illustrates that large, unidentified l3 values can confound attempts to recover system parameters from photometry alone.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Posterior probabilities on a subset of system parameters for J082700.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: A histogram showing how much more the secondaries in close-binary systems (P < 2 days) fill their Roche lobes compared to their respective primaries for the 16 detached and semidetached systems in C23 and the current paper.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Temperature ratio vs. ﹩\mathrm{log}q﹩ for 16 detached and semidetached systems. The open circles are systems from C23 and the filled circles are the detached systems in the present paper. The solid line is a power-law fit to the results. The other lines show the expected trend for pairs of main-sequence stars with G0V, F0V, and A0V primaries (dashed, dashed–dotted, and dotted lines, respectively).
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Relationship between TRIPOL g-band flare energies and FWHM temperatures for the M dwarfs’ flares. Black dots represent flares observed on Wolf 359 in this study. Gray dots are flares from field M dwarfs reported by W. S. Howard et al. (2020). TRAPPIST-1 flares are shown as yellow and blue dots, corresponding to data from A. J. Maas et al. (2022) and W. S. Howard et al. (2023), respectively. The green dashed lines show the power-law correlations derived from M dwarf superflares reported by W. S. Howard et al. (2020). The purple dashed lines represent the power-law correlations derived from low-energy Wolf 359’s flares reported in this study and Trappist-1’s flares reported in A. J. Maas et al. (2022) and W. S. Howard et al. (2023) (see Equation (8) and the coefficients in Table 7). The subpanels below each panel show the residuals diagrams relative to the solar-class flare power laws, visually demonstrating the goodness of fit for flares across all energy regimes.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Cumulative frequency distributions of flare temperatures for Wolf 359. Top: flare FWHM temperature distribution (Tfl,fwhm). Bottom: global flare temperature distribution (Tfl,glob). In both panels, the cumulative number of flares per year is plotted as a function of temperature, with the blue dashed lines showing the best-fit power-law relations. The fitted slopes are −2.92 ± 0.31 for Tfl,fwhm and −2.87 ± 0.21 for Tfl,glob. We note that these empirically derived slopes of the flare temperature frequency distributions may be biased and shallower than what they should be due to the limited sample size. A more complete and statistically robust flare data set will be crucial for more accurately constraining its underlying power-law behavior.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: TRIPOL g-band (green) response factor as the function of blackbody temperature. The Evryscope ﹩{g}^{{\prime} }﹩-band response factor function (orange) from W. S. Howard et al. (2020) is displayed for comparison.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: The fraction of bolometric flare energy emitted within the PAR wavelength range as function of flare temperature, ϵPAR(Tfl), we employ in Equation (11).
Paper: Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration
Authors: Yugo Kawai, Akihiko Fukui, Noriharu Watanabe, Sho Fukazawa, Norio Narita
Figure caption: System parameters as a function of dynamical age, τcir/τage, for planets with e < 0.1 (including those on assumed circular orbits). The vertical line marks the threshold for disk migration candidates. Points are color-coded by mass ratio in quartiles, with four shades of green: darkest for the top 25% (75–100th percentile), medium-dark for 50–75th, medium-light for 25–50th, and lightest for 0–25th. Gray points denote systems with only upper limits on mass ratio. Double-filled circles indicate nearby companions, and circles filled with diamonds indicate systems with known binary companions. Gray and white histograms show distributions for dynamically old and young systems, respectively. For clarity, error bars on dynamical age are shown only for disk migration candidates. In the semimajor axis and orbital period panels, horizontal dashed lines mark a = 0.1 au and P = 10 days; diagonal lines trace expected dynamical age assuming median system values. The entire plot or individual panels can be regenerated with ident-dm (https://github.com/ykawai6581/ident_dm; doi:10.5281/zenodo.17100956).
Paper: Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration
Authors: Yugo Kawai, Akihiko Fukui, Noriharu Watanabe, Sho Fukazawa, Norio Narita
Figure caption: Top: p-values from KS tests with trial Qp comparing the eccentricity distributions of dynamically old and young planets across four representative iterations (out of 3000 total), distinguished by different line styles. In each curve, the minimum p-value among the trial Qp values in the same iteration is marked with an “x.” Bottom three panels: histograms of Qp corresponding to the locations of minimum p-values in each of the 3000 iterations, shown for (1) all planets, (2) planets above the median mass (Mp > 0.96 MJ), and (3) those below. In the first panel, we also overlay the case with a 3 Gyr offset applied to τcir, simulating the delay introduced by preceding processes such as eccentricity excitation. Dotted lines and blue shading indicate the constraints on QJ, while dashed lines and orange shading show constraints on Qp from S. N. Quinn et al. (2014).
Paper: Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration
Authors: Yugo Kawai, Akihiko Fukui, Noriharu Watanabe, Sho Fukazawa, Norio Narita
Figure caption: A recreation of Figure 4 in S. N. Quinn et al. (2014). The system age τage is plotted against the tidal circularization timescale τcir in logarithmic space, with color contours indicating orbital eccentricity. The dashed line marks where τcir = τage, based on Qp = 4.9 × 105. The shaded region reflects the uncertainty in Qp. Marker size corresponds to planetary mass, and planets with only mass upper limits are excluded. Planets with fully constrained eccentricities are shown as circles, those with upper limits are triangles, and assumed circular orbits are indicated by squares. Dynamically old but eccentric outliers are highlighted in orange, while disk migration candidate hot Jupiters (a < 0.1 au) are highlighted in blue. We note that ﹩{({\tau }_{{\rm{cir}}}/{\tau }_{{\rm{age}}})}_{{\rm{median}}}\gt 1﹩ does not strictly imply τcir,median/τage,median > 1, and vice versa. This results in one planet to the left of the dashed line being highlighted in blue, and another to the right not being highlighted.
Paper: Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration
Authors: Yugo Kawai, Akihiko Fukui, Noriharu Watanabe, Sho Fukazawa, Norio Narita
Figure caption: The result of the Monte Carlo experiment described in Section 4.2. While the sample of seven hot Jupiters with nearby companions contains an average of 3.83 dynamically young systems, a sample of seven randomly drawn hot Jupiters on circular orbits typically contains none. The resulting p-value is 0.001, corresponding to 3.1σ.
Paper: Identifying Close-in Jupiters that Arrived via Disk Migration: Evidence of Primordial Alignment, Preference of Nearby Companions and Hint of Runaway Migration
Authors: Yugo Kawai, Akihiko Fukui, Noriharu Watanabe, Sho Fukazawa, Norio Narita
Figure caption: The marginalized posterior density ﹩{\mathrm{log}}q﹩ for dynamically old and young systems on circular orbits.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Nobeyama 12CO J = 1–0 intensity maps integrated each 1.3 km s−1 in the velocity range of +30.33–+41.38 km s−1, overlaid by the contours of the radio continuum flux density at an effective frequency of 1.36 GHz. The red circle marked in the +30.65 km s−1 panel represents the region from which the CO line spectra in Figure 1 are extracted. The red boxes labeled “NE” and “SW” are used to inspect the 12CO J = 1–0 and 13CO J = 1–0 spectrum grids (see Figures 4 and 5).
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Grid of PMOD 12CO J = 1–0 and 13CO J = 1–0 lines in the velocity range of +35–+47 km s−1 for region “NE” as labeled in Figure 2. The black curves are 12CO spectra and the red curves are 13CO spectra. The horizontal dashed lines denote the 0 K main-beam temperature. The black contours are the same as those in Figure 2. The size of each pixel is 30″ × 30″. The region delineated by the green rectangle (labeled “1”) is used to extract the CO spectra presented in Figure 6, in which redward broadened wings for the 12CO emission are shown at VLSR ∼ 40 km s−1.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Grid of PMOD 12CO J = 1–0 and 13CO J = 1–0 lines in the velocity range of +30–+40 km s−1 for region “SW” as labeled in Figure 2. The black, red, and horizontal dashed lines are the same as in Figure 4. The black contours are the same as those in Figure 2. The size of each pixel is 30″ × 30″. The regions delineated by the green rectangles (labeled “2” and “3”) are used to extract the CO spectra presented in Figure 6, in which redward broadened wings for the 12CO emission are shown at VLSR ∼ 33 km s−1.