adsabs/AstroCLIMB huggingface dataset:
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 continuum image. The contours are 10σ, 20σ, 40σ, 80σ, 160σ, and 320σ (1σ = 0.11 mJy beam−1). The red and blue arrows denote the outflow directions of the red- and blueshifted components, respectively, in a small scale in the vicinity of HOPS 373SW. The inset presents the integrated intensity map of the averaged CH3OH (color image) with the same contours for the continuum intensity. The CH3OH intensity is integrated within ±1 km s−1 after correcting for the envelope velocity profile using the 13CH3OH intensity-weighted velocity map (second panel in the top row of Figure 2), and only the integrated intensity over 5σ (1σ = 1.1 mJy beam−1 km s−1) is presented in the color image. The observed beam is presented by the filled black ellipse in the top left corner.
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: Spectra of HOPS 373SW fitted with XCLASS. Different colors represent the line transitions of different species. Black solid/dashed lines represent the tentatively identified lines. The C2H5OH lines are largely blended with other species. Thus, to clearly distinguish them, we shaded the C2H5OH lines in orange. The identified lines are listed in Tables 2 and 3, and the column density and excitation temperature best fitted for each species are summarized in Table 4 along with the abundance relative to CH3OH. The dashed and dotted horizontal lines represent the 1﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ and 3﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ levels, respectively.
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: Integrated intensity map (color) of the C5H line at 336.5148 GHz (left) and the spectra extracted from the full circle and western semicircle as marked in black and orange, respectively, in Figure 3 (right). The emission distributes only in the eastern part of HOPS 373SW, where the lines are affected by outflows/jets. Therefore, the C5H line disappears in the spectrum extracted from the western semicircle (right). In the left panel, the contours show the distribution of the dust continuum emission, and the levels are the same as those in Figure 1. The integrated intensity over 5σ (1σ = 1.96 mJy beam−1 km s−1) is presented in the color image. The dashed and dotted lines in the right panel represent the 3﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ and 5﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ (1﹩{\sigma }_{{T}_{\mathrm{mb}}}﹩ = 2.2 K) levels, respectively.
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: Excitation diagrams of CH3OH (v  t  = 2), CH2DOH, CHD2OH, CD3OH, 13CH3OH, CH3CN, CH3CHO, and C2H5OH. The isolated lines that can be fitted with a Gaussian profile are used for these excitation diagrams.
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: Position–velocity diagram of 13CH3OH along the decl. The plus sign indicates the source velocity (10.13 km s−1) and continuum peak position. The contours are 5σ, 8σ, and 11σ (1σ = 1.8 mJy beam−1).
Paper: Five Massive Contact Binaries with Twin Components in LMC
Authors: Fu-Xing Li, Sheng-Bang Qian, Chu-Qi Wu, Min-Yu Li, Er-Gang Zhao, Wen-Ping Liao, Li-Ying Zhu, Qi-Bin Sun, Jia Zhang
Figure caption: The (O − C) diagrams for five binaries. The upper plots of each panel represent the (O − C) curves with all minima (the blue solid circles and the orange solid circles are the primary and secondary minima, respectively) calculated by the linear ephemerides, while the black lines refer to the trend of (O − C) values. The middle and lower plots of each panel represent the cyclic oscillations and the residuals, respectively.
Paper: Five Massive Contact Binaries with Twin Components in LMC
Authors: Fu-Xing Li, Sheng-Bang Qian, Chu-Qi Wu, Min-Yu Li, Er-Gang Zhao, Wen-Ping Liao, Li-Ying Zhu, Qi-Bin Sun, Jia Zhang
Figure caption: The q-search diagrams. Panel (a) refers to the q-search of four binaries (S02776, S12878, S15994, and S18865). Panel (b) is the residual curves of S19959, which are the combined solution of multiband (V, I) and the independent solutions of V and I bands, respectively.
Paper: Five Massive Contact Binaries with Twin Components in LMC
Authors: Fu-Xing Li, Sheng-Bang Qian, Chu-Qi Wu, Min-Yu Li, Er-Gang Zhao, Wen-Ping Liao, Li-Ying Zhu, Qi-Bin Sun, Jia Zhang
Figure caption: The solid lines (the pink and blue ones refer to the I band and V band, respectively) and black points represent the theoretical and observational light curves for five binaries in the LMC; points in the lower subpanels in each panel represent the corresponding residual.
Paper: Five Massive Contact Binaries with Twin Components in LMC
Authors: Fu-Xing Li, Sheng-Bang Qian, Chu-Qi Wu, Min-Yu Li, Er-Gang Zhao, Wen-Ping Liao, Li-Ying Zhu, Qi-Bin Sun, Jia Zhang
Figure caption: Eclipse time of S18865.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Deflection distributions for CMEs with ∣latitude∣ ≤ 30° (panel (a)), with 30°<∣latitude∣ < 60° (panel (b)) and ∣latitude∣ ≥ 60° CMEs (panel (c)). In the upper left corner of each panel, the basic parameters of these distributions are presented. Dashed lines represent a Gaussian fitting to histograms obtained from observations.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Distributions of yearly averaged deflections (PAi-PAF) of all considered CMEs (panel (a)), CMEs from the northern hemisphere (panel (b)), and CMEs from the southern hemisphere (panel (c)). Light gray bars represent negative and positive deflection separately. Dark gray bars are for both kinds of deflection together. The dashed vertical lines represent solar cycle boundaries.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Sample trajectories of three CMEs (distance from the Sun vs. PA) illustrate deflection toward the equator (dotted line, 20010819.060605), the pole (dashed line, 20040519.202605), and no deflection (continuous line, 20100413.083005). The dotted lines indicate the initial and final PAs of the respective CMEs. Figure illustrates the field of view of LASCO coronographs for position angles from 270° to 360°. In the bottom left corner, the solar surface is marked.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Deflection distributions (PAi-PAF) for all considered CMEs (panel (a)), all CMEs in solar cycle 23 (panel (b)), and all CMEs in solar cycle 24 (panel (c)). In the upper left corner of each panel, the basic parameters of these distributions are presented. Dashed lines represent a Gaussian fitting to histograms obtained from observations.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Deflection distributions for CMEs with the angular width >30° (panel (a)), with the angular width >60° (panel (b)), and with the angular width >120° (panel (c)). In the upper left corner of each panel, the basic parameters of these distributions are presented. Dashed lines represent a Gaussian fitting to histograms obtained from observations.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Distributions of yearly averaged deflection at 5R ⊙ (panel (a)), at 10R ⊙ (panel (b)), and at 20R ⊙ (panel (c)). Light gray bars represent negative and positive deflection separately. Dark gray bars are for both kinds of deflection together. The dashed vertical lines represent solar cycle boundaries.
Paper: A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs
Authors: Grzegorz Michalek, Nat Gopalswamy, Seiji Yashiro, Kostadinka Koleva
Figure caption: Deflection distributions for slow CMEs (speed ≤ 400 km s−1, panel (a)), mid-speed CMEs (400 km s−1 < speed ≤ 800 km s−1, panel (b)) and fast CMEs (speed > 800 km s−1, panel (c)). In the upper left corner of each panel, the basic parameters of these distributions are presented. Dashed lines represent a Gaussian fitting to histograms obtained from observations.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of the long lags detected by JAVELIN for 100 mock long season cadence LSST light curves with input long lags, shown by the dashed vertical lines, of −50 days (top panel), −130 days (middle panel), and −400 days (bottom panel). Distributions shown in blue also include a short lag of 7 days (top panel), 9 days (middle panel), and 14 days (bottom panel). The ratio of the amplitude of the long lag to the amplitude of the short lag is shown in the legends for each blue distribution.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the short lag recovered by the maximum-likelihood method for 100 mock light curves with input lags of −50 and 7 days. The dashed vertical line shows the input short lag. The green and light blue distributions are for mock light curves with the baseline v2.0 LSST cadence for the u and y band and g and z band, respectively. The distributions shown in pink are for light curves with the baseline g- and z-band cadence plus an LCO observation taken roughly every 10 days in each LSST observing gap. These LCO observations amount to around 18 observations in each gap, or per year, for a total of around 180 observations.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lags recovered by the maximum-likelihood method for 100 mock long season cadence LSST light curves with input long lags, shown by the dashed vertical lines, of −50 days (top panel) and −130 days (bottom panel). Distributions shown in blue also include a short lag of 7 days (top panel) and 9 days (bottom panel). The ratio of the amplitude of the long lag to the amplitude of the short lag is shown in the legends for each blue distribution.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distributions of the long lags recovered by JAVELIN for 100 mock light curves with the long season LSST cadence and input lags of −50 and 7 days (top panel), −130 and 9 days (middle panel), and −400 and 12 days (bottom panel). The vertical dashed lines show the input long lag. The colored lines are the distributions for light curves where we set i = 21 to explore how a lower S/N changes our ability to detect lags. The distributions of these lags are very similar to the distributions shown in gray, which are for light curves with the i-band magnitudes in Table 1.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distributions of the long lags recovered by the maximum-likelihood method for 100 mock light curves with the long season LSST cadence and input lags of −50 and 7 days (top panel) and −130 and 9 days (bottom panel). The vertical dashed lines show the input long lag. The colored lines are the distributions for light curves where we set i = 21 to explore how a lower S/N changes our ability to detect lags. The distributions of these lags are very similar to the distributions shown in gray, which are for light curves with the i-band magnitudes in Table 1.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lags recovered by JAVELIN for 16 mock long season cadence LSST light curves made using light curves from the simulation in Jiang & Blaes (2020) for input lags of −50 and 7 days (top panel), −130 and 9 days (middle panel), and −400 and 12 days (bottom panel). The long lags are shown as the dashed vertical line.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lags detected by the maximum-likelihood method for 16 mock long season cadence LSST light curves made using light curves from the simulation in Jiang & Blaes (2020) for input lags of −50 and 7 days (top panel) and −130 and 9 days (bottom panel). The long lags are shown as the dashed vertical line.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lag recovered by the Von-Neumann method for 100 mock light curves with input lags of −50 and 7 days. The dashed vertical line shows the input long lag. The orange (green) distribution is for mock light curves with the long season (baseline u and y band) cadence.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the short lags detected by the maximum-likelihood method for 16 mock long season cadence LSST light curves made using light curves from the simulation in Jiang & Blaes (2020) for input lags of −50 and 7 days (top panel) and −130 and 9 days (bottom panel). The short lags are shown as the dashed vertical line.
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Unveiling the Driving and Constraining Forces
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Distribution of Lorentz force and Lorentz force work in the slow-rise phase. (a) Distribution of quashing factor Q on an x–z plane located at y = 49.92 Mm at t = 639.85 s. The purple and blue contours show the quashing factor with a level of log Q = 3 and the twist number with a level of T  w  = −1.5, respectively. (b) Distribution of the z-component of Lorentz force on the same plane as that in (a) at t = 639.85 s. The purple contour shows the current density with a level of j = 2 × 10−7 G cm−1. The magnetic field lines before and after magnetic reconnection as well as that selected within the flux rope are projected on the plane as green, orange, and blue dotted–dashed lines, respectively. The horizontal red dashed lines in both (a) and (b) mark the height of the lower boundary of the flux rope on this plane. (c) Height–time diagram of the Lorentz force work (color bar) integrated within each horizontal layer with the height of one pixel. The blue contour marks the value of P = 8 × 1024 erg s−1. The higher and lower red dotted lines mark the average lower and upper boundaries of the flux rope, respectively. The time of the snapshot shown in (a) and (b) is indicated by the black vertical dashed line, while the onset time t  b  is indicated by the white vertical dashed line.
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Unveiling the Driving and Constraining Forces
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Cartoon of the confined eruption describing the evolution of the flux rope before and during the eruption. (a) The slow-rise phase of the flux rope. (b) Eruption of the flux rope. (c) Confinement of the eruption. The gray plane marks the photosphere, where the white and black dotted circles correspond to the positive and negative magnetic poles, respectively. The purple tube surrounded by a group of purple lines marks the main body of the magnetic flux rope. The yellow and orange lines mark the magnetic arcades in the lower corona, while the higher arcades are drawn as dark green lines. The white arrow marks the toroidal current J t within the flux rope, while the light blue one surrounding the flux rope in (c) indicates the poloidal current J p of it. The red pentagrams indicate the reconnection site. The dark red, light green, and dark blue arrows at the bottom left corner refer to the x-, y-, and z-axes, respectively. See Section 5 for more details.
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Unveiling the Driving and Constraining Forces
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Acceleration of the flux rope compared with the evolution of reconnection efficiency. The numerical resistive dissipation term ﹩{Q}_{\mathrm{res}}﹩ integrated within a region containing the current sheet under the flux rope (blue) and the derivative of synthetic GOES flux (red) are used as proxies of the reconnection efficiency. The acceleration is the same as that in Figure 2(d).
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Unveiling the Driving and Constraining Forces
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Distribution of forces across the flux rope along S1 at t = 780.81 s when the flux rope is decelerating. The red line presents the Lorentz force, and the gravity multiplied by 50 is shown by the blue line.
Paper: Deep Search for Molecular Oxygen in TW Hya
Authors: Becky J. Williams, L. Ilsedore Cleeves, Christian Eistrup, Jon P. Ramsey
Figure caption: Matched filtering response for the 16O18O data, with impulse response on the y-axis and velocity on the x-axis. The 233.946 GHz transition is centered at 0 km s−1 and is denoted by the vertical dashed line. The two horizontal lines are at 0σ and 3σ. The gray region in the left plots is the range of velocities covered in the right plots. (a) 120 au filter, covering all channels. (b) Zoom-in of the shaded region in panel (a). (c) 260 au filter, covering all channels. (d) Zoom-in of the shaded region in panel (c).
Paper: Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Unveiling the Driving and Constraining Forces
Authors: Can Wang, Feng Chen, Mingde Ding, Zekun Lu
Figure caption: Decay index calculated with the full horizontal component of the potential field, which includes both the poloidal component and the toroidal component. The gray dotted and dashed lines indicate the value of the decay index at 1 and 1.5, respectively.
Paper: Deep Search for Molecular Oxygen in TW Hya
Authors: Becky J. Williams, L. Ilsedore Cleeves, Christian Eistrup, Jon P. Ramsey
Figure caption: Channel maps of the intensity, centered on 233.946 GHz. The systemic velocity is 2.86 km s−1. The two Keplerian masks are shown in white contours, and velocities are shown in the lower right of each panel. The beam size is 0.″59 × 0.″50 and is shown in the lower left panel.
Paper: Deep Search for Molecular Oxygen in TW Hya
Authors: Becky J. Williams, L. Ilsedore Cleeves, Christian Eistrup, Jon P. Ramsey
Figure caption: Spectrum of the O2 data for TW Hya, calculated within a 260 au region. The dashed line is the systemic velocity of 2.86 km s−1, centered on 233.946 GHz.
Paper: First Results for Solar Soft X-Ray Irradiance Measurements from the Third-generation Miniature X-Ray Solar Spectrometer
Authors: Thomas N. Woods, Bennet Schwab, Robert Sewell, Anant Kumar Telikicherla Kandala, James Paul Mason, Amir Caspi, Thomas Eden, Amal Chandran, Phillip C. Chamberlin, Andrew R. Jones, Richard Kohnert, Christopher S. Moore, Stanley C. Solomon, Harry Warren
Figure caption: Example DAXSS solar spectra from 2022 April 24 (DOY 114) for quiescent-Sun (preflare, or PF, at 9:05 UT; black), flare (C2 flare at 11:00 UT; red), and occultation (OCC at 11:14 UT; blue) data. The occultation data are defined as the time when the solar-viewing tangent ray height is below 300 km, and they are indicated as the data between the vertical blue lines in panel (A). The spectra in panel (B) are 1 minute averages of the DAXSS Level 0D count-rate spectra. The flare irradiance spectrum in panel (C) is from the DAXSS Level 1 product, with the preflare 9:05 UT spectrum subtracted from the flare spectrum at 11:00 UT. The solar occultation spectrum is when the tangent ray height is about 103 km and the solar zenith angle is about 110°, and the ratio shown in panel (D) illustrates the amount of atmospheric absorption as a function of energy (wavelength).
Paper: First Results for Solar Soft X-Ray Irradiance Measurements from the Third-generation Miniature X-Ray Solar Spectrometer
Authors: Thomas N. Woods, Bennet Schwab, Robert Sewell, Anant Kumar Telikicherla Kandala, James Paul Mason, Amir Caspi, Thomas Eden, Amal Chandran, Phillip C. Chamberlin, Andrew R. Jones, Richard Kohnert, Christopher S. Moore, Stanley C. Solomon, Harry Warren
Figure caption: Example DAXSS solar occultation is illustrated for an experiment done on 2022 April 24 near 10 UT. Panels (a) and (b) show occultation geometry cartoons for the beginning of the occultation (gold) and at the minimum tangent ray height (green), respectively. The occultation profiles at four different energies are shown in panel (d), using the DAXSS Level 0D data product (9 s cadence) over a 22 minutes period while the spacecraft went over Earth’s south pole. As illustrated in panel (c), the black symbols are the spacecraft position, the red symbols are the location of the tangent ray point, the gold symbols are the starting points, and the green symbols are at the time of the minimum tangent ray height. The view of the globe is rotated so that the solar direction is straight up at the time of the minimum tangent ray height. The absorption profiles in panel (d) are normalized by the signal at the tangent ray height of 300 km and are also corrected for solar variability, using the GOES XRS-B irradiance as a variability proxy. These profiles are not corrected for the different locations over Earth that changed by 169° in longitude and by 37° in latitude. The down-leg is the upper trace of the profiles. The spacecraft altitude and the solar zenith angle are fairly constant, with averages of 542 km and 108°, respectively.