adsabs/AstroCLIMB huggingface dataset:
Paper: Nitrogen as a Tracer of Giant Planet Formation. II. Comprehensive Study of Nitrogen Photochemistry and Implications for Observing NH3 and HCN in Transmission and Emission Spectra
Authors: Kazumasa Ohno, Jonathan J. Fortney
Figure caption: Emission spectra of 1 Gyr old Jupiter-mass planets with T eq = 800 K around Sun-like stars for various values of eddy diffusion strength K zz (left column) and atmospheric metallicity (right column).
Paper: Nitrogen as a Tracer of Giant Planet Formation. II. Comprehensive Study of Nitrogen Photochemistry and Implications for Observing NH3 and HCN in Transmission and Emission Spectra
Authors: Kazumasa Ohno, Jonathan J. Fortney
Figure caption: Transmission spectra of a 1 Gyr old Jupiter-mass planet with T eq = 800 K around Sun-like stars for various K zz values (left) and atmospheric metallicities (right).
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: (Left panel) Example simulation showing the distance residuals to 40 calibrator galaxies with sibling pairs, where the true σ Rel = σ 0/2 = 0.05 mag. The distance residual, ﹩{\hat{\mu }}_{\mathrm{Calib}.}-{\mu }_{\mathrm{True}}^{\mathrm{Sim}}﹩, compares the true distance in the simulation, ﹩{\mu }_{\mathrm{True}}^{\mathrm{Sim}}﹩, with the calibrated SN siblings' common distance estimate to the calibrator galaxy, ﹩{\hat{\mu }}_{\mathrm{Calib}.}﹩. (right panel) We plot a KDE of the 40 distance residuals, ﹩| {\hat{\mu }}_{\mathrm{Calib}.}-{\mu }_{\mathrm{True}}^{\mathrm{Sim}}| /{\hat{\sigma }}_{\mu }﹩, averaged over 100 simulations, which shows how well-estimated the calibrator galaxy distance uncertainties are. For each galaxy, we take the posterior median distance estimate and divide by the posterior standard deviation, ﹩{\hat{\sigma }}_{\mu };﹩ the vertical lines show the 68% quantiles, which should be close to unity if the uncertainties are well estimated. The uncertainties are overestimated when adopting the δ M-Common assumption (where σ Rel = 0 is assumed), whereas the δ M-Uncorrelated uncertainties are underestimated (where σ Rel = σ 0 is assumed). The δ M-Mixed results (where σ Rel is marginalized over) and the δ M-True results (where σ Rel is known and fixed in the model fit) agree with one another; moreover, the 68% quantiles are strongly consistent with unity, indicating the distance uncertainties are well-calibrated.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Magnetograms used in all of the different simulations and a schematic representation of the magnetic null point. (A) Magnetic flux distribution and surface rotation flow at the bottom boundary (i.e., z = 0). The background is color-coded by the vertical magnetic component B  z , and the vectors show the rotational flow. The blue and red lines represent half of the maximum and minimum values of the vertical magnetic components B  z  on the bottom, respectively. The format of panels (B), (C), (D), and (E) is the same as that of panel (A) but without showing the rotational flow. The name of the magnetogram and the height of the magnetic null point are also marked in each panel. (F) Potential field structure obtained by extrapolation using magnetogram M1. The thick curves with different colors represent magnetic field lines belonging to different flux systems that meet at the X point, i.e., the magnetic null point. The yellow lines are contours of B  z .
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: (Left panel) Rest-frame light curves in BgVrizYJH passbands are synthesized using the new W22 BAYESN model, to illustrate the intrinsic effect of W 1(t, λ), the first functional principal component (FPC). Dust extinction and residual functions are set to zero, and the coefficient on the first FPC, θ, is varied about the population mean; this variation gives rise to the Phillips (1993) “broader–brighter” empirical relation in optical passbands, while also affecting the NIR amplitudes and times of the second peak. For visual clarity, the BgVrizYJH light curves have been vertically offset by (1.25, 0, −1, −2.25, −4, 2.5, 0.25, −2.75, −4) mag, respectively. (right panel) Rest-frame intrinsic color curves are synthesized using the new W22 BAYESN model, to illustrate the predicted level of residual intrinsic color variation after correction for dust extinction and light-curve shape. Dust extinction and the light-curve shape, θ, are set to zero. The solid black lines depict the mean intrinsic color curves, while the dashed lines show a 1 σ variation about the mean, computed by taking the standard deviation of many residual function realizations, each drawn from the intrinsic SED residual covariance matrix. For visual clarity, the colors are offset by (−0.75, 0.25, 1.25, 2.5, 3.5, 0.25, 2.25, 3.25) mag for (B − V, g − V, V − r, V − i, V − z, V − Y, V − J, V − H), respectively.
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: Chromatic parameter uncertainties are affected in the opposite sense to the distance hyperparameter by different intrinsic scatter modeling assumptions (Table 3). The overlay shows distance and common-R  V  posteriors from individual fits [colors] and joint fits [black]. (top panel) Assuming the siblings are uncorrelated minimizes the distance estimate uncertainty, while marginalizing over σ Rel yields robust uncertainties. (bottom panel) The common-R  V  posteriors [black] show that the more correlated the intrinsic scatter components are, the less freedom there is in the fit, which results in tighter constraints on chromatic parameters. This is opposite to the behavior of the distance hyperparameter. Marginalizing over σ Rel yields R  V  = 2.62 ± 0.67.
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: Hubble constant inference from simultaneously fitting NGC 3147's siblings’ light curves, the Cepheid distance from Riess et al. (2022), and BAYESN distance estimates to 109 SNe Ia in the Hubble flow. We marginalize over the total intrinsic scatter, σ 0, the siblings’ relative intrinsic scatter, σ Rel, and the peculiar velocity dispersion, σ pec. Marginalizing over σ Rel while jointly fitting the siblings’ light curves yields the best NGC 3147 distance constraint. We estimate H 0 = 78.4 ± 6.5 km s−1 Mpc−1.
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: Spectrum of SN 2021hpr, observed ≈4.2 days before the B-band maximum, using the Kast spectrograph on the Lick Shane telescope, in the observer-frame wavelength range: 3254–10894 Å.
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: Individual BAYESN fits to SNe 1997bq and 2008fv (as in Figure 2). R  V  posteriors are wide owing to the moderate extinction and lack of NIR data.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Formation process of the core CS. (A) Distribution of normalized current J/B on the x = 0 slice in simulation M1. (B) 1D profile of the magnetic component B  z  and normalized current density along the horizontal line perpendicular to the center of the core CS (location with the maximum J/B). The diamonds represent the value on the grid nodes. The thin black line is a Gaussian function fitting of the normalized current density J/B profile, and its FWHM is used to measure the thickness of the CS. (C) Temporal evolution of the thickness of the core CS in five simulations. The time axes of all of the simulations are shifted so that t = 0 denotes the onset of eruption, as shown by the vertical dashed line. Each circle represents a moment of output data, and a higher time resolution is used near the eruption onset. The maximum speeds of the core CS thinning in M1 and M0 are also denoted by the dotted lines and numbers.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Pre-eruption evolution of the magnetic field line anchored at the center of the positive polarity of the core field. The rising of the apex of this field line is used to indicate the expansion of the core field. (A) In simulation M1, the evolution of the projection of the magnetic field line on the x = 0 plane. (B) The apex of the magnetic field line varies with time in five simulations. The vertical dashed lines denote the onsets of the eruption. (C) Rising speed of the apex in the five simulations.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Temporal evolution of the thickness of the current layer that formed in the core field in nine driving-stopped simulations. Panels (A), (B), and (C) represent simulations M0, M1, and M3, respectively. The details are similar to those in Figure 4(c). The thickness of the current layer is defined as the thickness at the maximum value of J/B or the thinnest part of the current layer morphology. Note that in panel (B), the core current layer is very thick before t = 80, so the number of grid nodes used for Gaussian function fitting in M1 is different from that in M1S3.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Temporal evolution of energies in nine driving-stopped simulations. (A) Evolution of magnetic energy E M (solid lines) and kinetic energy E K (dotted lines). Red, blue, and green in each panel denote the simulation with driving stopped at different moments (S1, S2, and S3, respectively). The vertical dashed lines denote the moments when driving stops. (B) Decreasing rate of magnetic energy and increasing rate of kinetic energy of six simulations that produce an eruption (S1 and S2). The vertical dashed lines with numbers show the onsets of the eruption.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Evolution of the specific magnetic field line and its height with time in nine driving-stopped simulations. Panels (A), (B), and (C) represent M0, M1, and M3, respectively. The details are similar to those in Figure 5.
Paper: Supernovae Origin for the Low-latitude Intermediate-velocity Arch and the North Celestial Pole Loop
Authors: J. T. Schmelz, G. L. Verschuur, A. Escorza, A. Jorissen
Figure caption: Area maps centered showing the details of the environment at different velocities using HI4PI data with a 2 km s−1 bandwidth. In each frame the red dashed circle highlights the approximate boundary of the low-velocity circular cavity. Panels (a)−(f) at −70, −66, −62, −58, −54, and −50 km s−1, respectively, show different velocity slices of the approaching shell. Legends in kelvins. Panel (g) at −2 km s−1 shows the NCP loop, as well as a circular structure with multiple extending threads in the lower left quadrant. Panel (h) at +2 km s−1 shows the complex circular cavity structure and a more defined image of the NCP loop. Panel (i) at +6 km s−1 shows a circular structure with multiple extending threads in the upper right quadrant, similar to the fainter structure seen in panel (g). Panel (j) at +10 km s−1 shows the first hints of the oval cavity (blue dashed ellipse) traditionally associated with the NCP loop. Panel (k) +14 km s−1 shows the lower arc at (l, b) = (143°, 25°) that helps define the oval cavity. Panel (l) at +18 km s−1 shows higher-velocity traces of the oval cavity. Legends in kelvins.
Paper: Supernovae Origin for the Low-latitude Intermediate-velocity Arch and the North Celestial Pole Loop
Authors: J. T. Schmelz, G. L. Verschuur, A. Escorza, A. Jorissen
Figure caption: (l, v) maps at different latitudes. (a) At b = 39°, the curvature of the H I emission around −50 to −60 km s−1 (the LLIV arch) is a signature of the structure on the near side of the expanding shell. The low-velocity gas shows a clear distortion. (b) At b = 37°, the emission from the shell is again well defined, bridging to low-velocity gas at around l = 131° and 170°. The bright feature at l = 125°, +5 km s−1 is part of the NCP loop. This map also shows the distortion of the low-velocity peak to positive velocities from l = 120° to 145°. The low-velocity gas has a wavelike velocity gradient from the location of the emission from the NCP loop area around l = 120° to the edge of the map at l = 180°. Panel (c) at b = 35° shows the continuity of the H I around −55 km s−1 linking with low-velocity gas at l = 130° and 170°. Emission from the NCP loop is still prominent at around l = 125°. Legends in kelvins.
Paper: Supernovae Origin for the Low-latitude Intermediate-velocity Arch and the North Celestial Pole Loop
Authors: J. T. Schmelz, G. L. Verschuur, A. Escorza, A. Jorissen
Figure caption:                         (b, v) maps at different longitudes. Panel (a) at l = 169° shows twin ridges of positive- and near-zero-velocity gas. The positive-velocity ridge may represent the receding component of the expanding shell. Panel (b) at l = 157° shows the H I ridge at −55 km s−1 known as the LLIV arch with a velocity gradient consistent with an H I shell expanding away from the source and toward the observer. Panel (c) at l = 147° shows that the shell structure is extremely clumpy. Legends in kelvins. Panel (d) at 143° cuts across the center of the shell outlined in Figure 1. The distortion of the low-velocity gas is consistent with expansion on the far side. (Note that the long, horizontal contour at 40.°9 is the galaxy M81.) (e) At 139°, the near side of the shell shows knots and clumps. A connection to low-velocity gas is apparent at about 33° and 46°. (f) At l = 133°, the bright structure at positive velocities up to +10 km s−1 is the NCP loop. Legends in kelvins.
Paper: Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability
Authors: Alan P. Boss, Shubham Kanodia
Figure caption: Cross sections after 100 yr of evolution for model M1-6-40-40. Top left: log density cross section along the rotation axis for the plane x = 0. Bottom Left: temperature cross section along the rotation axis for the plane x = 0. Temperatures range from about 85 K (dark blue) at the disk midplane to about 240 K (yellow) in the regions above and below the disk. Top right: log density cross section in the disk midplane (z = 0) showing two gas giant protoplanets in the inner disk, one at 1 o’clock with a mass of 2.5 M Jup and one at 8 o’clock with a mass of 5.5 M Jup. The sink particle at 11 o’clock has a mass less than 0.1 M Jup and so is not tabulated. Dense clumps that have not formed sink particles can be seen as well, e.g., at 10 o’clock. Bottom right: temperature cross section in the disk midplane (z = 0). Midplane temperatures range from about 85 K (dark blue) to about 100 K (yellow).
Paper: Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability
Authors: Alan P. Boss, Shubham Kanodia
Figure caption: Initial log density cross section in a vertical section (x = 0) on the left, and in the disk midplane (z = 0) on the right, showing the entire computational grid with a maximum of six levels of refinement for model M1-6-40-40, a 0.04 M ⊙ disk in orbit around a 0.5 M ⊙ protostar.
Paper: Supernovae Origin for the Low-latitude Intermediate-velocity Arch and the North Celestial Pole Loop
Authors: J. T. Schmelz, G. L. Verschuur, A. Escorza, A. Jorissen
Figure caption: Polar projection at around l = 135° shown in a schematic of the two cavities seen in Figure 4. The solid black circle represents the circular cavity, and the dashed ellipse depicts the oval cavity with the scale based on the suggestion by Marchal & Martin (2023). Gaia DR3 1093757200530267520 (system #25), at a distance of 207 pc (Table 2), sets the scale for the circular cavity. Several binary systems with potential neutron stars in orbit (see text) lie within the outlines of the oval cavity, which would account for its elongation along the line of sight. Also indicated are two regions where the circular cavity and the oval cavity interact—the NCP loop in red, and the lower arc in blue.
Paper: Supernovae Origin for the Low-latitude Intermediate-velocity Arch and the North Celestial Pole Loop
Authors: J. T. Schmelz, G. L. Verschuur, A. Escorza, A. Jorissen
Figure caption:                         A schematic showing the intersection of the two cavities as seen in Figure 1(k) at −14 km s−1. The red dashed circle depicts the circular cavity, and the blue dashed ellipse depicts the oval cavity. The locations of the spectroscopic binary systems at distances closer than 700 pc are indicated by red filled diamonds, with the adjacent numbers referring to the entries in Tables 2–4. The two binary systems of greatest interest are Gaia DR3 1093757200530267520 (system #25), close to the center of the circular cavity, and Gaia DR3 1144019690966028928 (system #13), close to the center of the oval cavity.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Overview of the COS G130M spectra obtained in the CLASSY survey with the wavelength coverage of 1170–1470 Å on the x-axis. The image is built by one continuum-normalized spectrum per image line. The redshift increases from top to bottom along the y-axis. The dark is low flux, and the yellow is high flux. The yellow waterfall highlights the redshifted Lyα emission lines. We use vertical white lines to mask the geocoronal Lyα and O II emission lines. The vertical dark lines indicate the MW absorption lines, and the gray strips indicate the CCD gaps.
Paper: Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW
Authors: Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Figure caption: ALMA Band 7 spectra of HOPS 373SW (gray solid lines) compared with those of V883 Ori (red dotted lines; Lee et al. 2019b). The spectral setup is almost the same in the two observations. The spectra of V883 Ori are extracted over the full annulus between 0.″1 and 0.″2 in radius, while the spectra of HOPS 373SW are extracted over the western semicircle between 0.″03 and 0.″1 (see Figure 3). The V883 Ori spectra have been scaled up by a factor of 4 to better compare with those of HOPS 373SW. The identified lines are marked with bars and symbols with different colors right above the individual lines. The newly detected lines in HOPS 373SW and the lines much stronger than those of V883 Ori are shaded; the gray shading denotes deuterated species, while the purple shading indicates unidentified or tentatively identified lines. The rms noises (﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩) are, before scaling up, 0.65 and 0.66 K for the spectral windows around 330 and 340 GHz, respectively, in V883 Ori. In HOPS 373SW, the rms noises (﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩) are 2.2 and 2.3 K for the spectral windows around 330 and 340 GHz, respectively. The red and gray dotted horizontal lines represent the 3﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ level.
Paper: Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW
Authors: Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Figure caption: Intensity-weighted velocity maps (colors) and integrated intensity maps (contours) of eight different molecular lines. Two isolated lines are each averaged for CH3OH, 13CH3OH, and CH3CHO. The start and step of the contours are 5σ. The rms noise levels are 1.1, 1.2, 2.1, 2.0, 2.3, 1.6, 1.9, and 2.3 mJy beam−1 km s−1 for CH3OH, 13CH3OH, CH2DOH, HDO, CH3CN, CH3CHO, CH3OCHO, and C2H5OH, respectively. The plus sign denotes the position of the continuum peak. The observed beam is presented in the lower left panel. A source velocity of 10.13 km s−1 is adopted.
Paper: Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW
Authors: Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Figure caption: Velocity dispersion (image) and the averaged spectra for the CH3OH and 13CH3OH lines. (a) The contours indicate the integrated intensity, and the start and step of the contours are 10σ. (b) The spectra are averaged within the regions outlined with the same colors (black, orange, and red) in the top panels. The vertical lines indicate the source velocity (10.13 km s−1) measured from the 13CH3OH spectra shown in the bottom right panel. Panels (c) and (d) are the same as panels (a) and (b) except for the CH3CN lines with two different upper energy levels.