adsabs/AstroCLIMB huggingface dataset:
Paper: VERTICO. VII. Environmental Quenching Caused by the Suppression of Molecular Gas Content and Star Formation Efficiency in Virgo Cluster Galaxies
Authors: Toby Brown, Ian D. Roberts, Mallory Thorp, Sara L. Ellison, Nikki Zabel, Christine D. Wilson, Yannick M. Bahé, Dhruv Bisaria, Alberto D. Bolatto, Alessandro Boselli, Aeree Chung, Luca Cortese, Barbara Catinella, Timothy A. Davis, María J. Jiménez-Donaire, Claudia D. P. Lagos, Bumhyun Lee, Laura C. Parker, Rory Smith, Kristine Spekkens, Adam R. H. Stevens, Vicente Villanueva, Adam B. Watts
Figure caption: The effect of environment—as traced by H I deficiency—on the rSFMS (top right), rMGMS (bottom left), and rKSR (bottom right) for the 15,401 pixels in our sample of 33 cluster galaxies. The same relations are shown for the resolution-matched HERACLES field sample (gray, 10,817 pixels, 10 galaxies). The distribution of H I deficiencies (top left) demonstrates the selection of the H I–poor (H I–def ≥ 0.5 dex, red) and H I–normal (H I–def < 0.5 dex, blue) subsamples. The relationships are shown using a Gaussian kernel density estimator with 10 isodensity contour levels linearly spaced between 5% and 100% of the distribution. The best fits are shown by the solid lines of corresponding color with the 1σ scatter illustrated by the shaded regions for the cluster subsamples and dashed lines for the field sample. Parameters and scatter of the best-fit relations are provided in Table 1 in the Appendix. The rSFMS and rMGMS in H I–normal galaxies follow the field relationships while the H I–poor galaxies have reduced SFR and molecular gas densities at fixed stellar mass.
Paper: Optical Identification of the Shortest-period Spider Pulsar System M71E
Authors: Zhuokai Liu, Subo Dong
Figure caption: Comparison between Pan23's favored binary evolutionary model and the observational constraints from HST photometry of COM-M71E in the Hertzsprung–Russell diagram. The blue curve is the evolutionary track presented in panel (A) of Extended Data Figure 4 of Pan23. The blue open circle shows the estimated properties (T eff ∼ 4500 K and luminosity L ∼ 3.25 × 10−3 L ⊙) of the companion by Pan23. The solid black line shows the T eff and L constraints from the M F606W derived from the HST optical detection, and the black dashed lines correspond to the 1σ range.
Paper: VERTICO. VII. Environmental Quenching Caused by the Suppression of Molecular Gas Content and Star Formation Efficiency in Virgo Cluster Galaxies
Authors: Toby Brown, Ian D. Roberts, Mallory Thorp, Sara L. Ellison, Nikki Zabel, Christine D. Wilson, Yannick M. Bahé, Dhruv Bisaria, Alberto D. Bolatto, Alessandro Boselli, Aeree Chung, Luca Cortese, Barbara Catinella, Timothy A. Davis, María J. Jiménez-Donaire, Claudia D. P. Lagos, Bumhyun Lee, Laura C. Parker, Rory Smith, Kristine Spekkens, Adam R. H. Stevens, Vicente Villanueva, Adam B. Watts
Figure caption: The distribution of galaxy H I deficiency for distinct RPS stages compiled from Yoon et al. (2017). The box shows the quartiles of the distribution while the whiskers extend to the full range in values. The number of galaxies in each stage is written next to the box. H I deficiency increases as RPS proceeds.
Paper: VERTICO. VII. Environmental Quenching Caused by the Suppression of Molecular Gas Content and Star Formation Efficiency in Virgo Cluster Galaxies
Authors: Toby Brown, Ian D. Roberts, Mallory Thorp, Sara L. Ellison, Nikki Zabel, Christine D. Wilson, Yannick M. Bahé, Dhruv Bisaria, Alberto D. Bolatto, Alessandro Boselli, Aeree Chung, Luca Cortese, Barbara Catinella, Timothy A. Davis, María J. Jiménez-Donaire, Claudia D. P. Lagos, Bumhyun Lee, Laura C. Parker, Rory Smith, Kristine Spekkens, Adam R. H. Stevens, Vicente Villanueva, Adam B. Watts
Figure caption: Median ΔSFE as a function of stellar mass surface density, Σ⋆ for the H I–normal (blue) and H I–poor (red) VERTICO cluster subsamples and HERACLES field sample (gray). Error bars illustrate ±1σ in each bin. The median ΔSFE (unbinned) for each subsample is shown by the dashed line of the corresponding color. Pixels belonging to H I–poor galaxies have lower SFEs at fixed stellar mass surface density.
Paper: VERTICO. VII. Environmental Quenching Caused by the Suppression of Molecular Gas Content and Star Formation Efficiency in Virgo Cluster Galaxies
Authors: Toby Brown, Ian D. Roberts, Mallory Thorp, Sara L. Ellison, Nikki Zabel, Christine D. Wilson, Yannick M. Bahé, Dhruv Bisaria, Alberto D. Bolatto, Alessandro Boselli, Aeree Chung, Luca Cortese, Barbara Catinella, Timothy A. Davis, María J. Jiménez-Donaire, Claudia D. P. Lagos, Bumhyun Lee, Laura C. Parker, Rory Smith, Kristine Spekkens, Adam R. H. Stevens, Vicente Villanueva, Adam B. Watts
Figure caption: Comparison of the resolved physical property distributions for the VERTICO cluster (blue) and HERACLES field (gray) samples. From left to right: molecular gas surface density (Σmol), stellar surface density (Σ⋆), SFR surface density (ΣSFR), and sSFR. All surface density properties are corrected for projection effects using the optical inclinations. As the cluster sample, regions in VERTICO galaxies are skewed to lower molecular gas and SFR densities.
Paper: Optical Identification of the Shortest-period Spider Pulsar System M71E
Authors: Zhuokai Liu, Subo Dong
Figure caption: A 5″ × 5″ section of the HST ACS F606W image around COM-M71E. The red circle is centered at the pulsar timing position of M71E, which agrees with the HST F606W position within ∼10 mas, and the circle’s radius is 10 times the HST astrometric error.
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—but only for 50 of the most deflected CMEs in a given year (light gray is for positive deflection and dark gray is for negative deflection). The white boxes show the maximal and minimal deflections recorded in a given year.
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 for narrow CMEs (widthle30°, panel (a)), mid-width CMEs (30° < widthle120°, panel (b)), and wide CMEs (width >120°, panel (a)).
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 for CMEs with ∣latitude∣ ≤ 20° (panel (a)), CMEs with 20° < ∣latitude∣ ≤ 79° (panel (b)), and CMEs with ∣latitude∣ > 70°, panel (a)).
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 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 (a)).
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 of all considered CMEs for PAi-PA05 (panel (a)), PAi-PA10 (panel (b)), and PAi-PA20 (panel (c)).
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: Scatter plot of deflection vs. speed for all considered CMEs. The dashed ones show roughly the limiting deflection values for the individual ejection velocities.
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: Scatter plots of deflection vs. CPA for all considered CMEs, for CMEs recorded in SC23, and for CMEs recorded in SC 24 and 25. Dashed lines represent polynomial fits to the data points.
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: Scatter plot of deflection vs. width for all considered CMEs.
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 normalized distribution of τ long(z) for quasars in SDSS DR7 (Shen et al. 2011) that fall within different redshift ranges. We assume α = 0.1, and take the masses, Eddington ratios, and redshifts from Shen et al. (2011). In the top left panel, we use β = 3.6 as in Yao et al. (2023); in the top right panel, we use β = 2, which is a more conservative estimate that the aspect ratio increases linearly with radius; in the bottom left panel, we use β = 0, and h/r = 0.01, which are typical values in the standard thin-disk model and lead to much long lag timescales (see different x-axis range); and in the bottom right panel, we use the ratios between the long and short lag for different wave bands in Yao et al. (2023).
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: Top panel: simulated driving u-band light curve, in blue, and y-band light curve, reprocessed with a long lag of −50 days, in orange. Middle panel: the same light curve as in the top panel subsampled using the long season LSST cadence. Bottom left: JAVELIN probability distribution for the long lag between the light curves above. The long lag is shown as a vertical dashed line. The median of the negative values of the distribution is −50 days. Bottom right: an example of the lags as a function of frequency recovered by the maximum-likelihood method for a mock light curve with an input long lag of −50 days (shown as the horizontal dashed blue line). The points are the lag detected in each bin (shown as the dashed vertical red lines). The vertical lines show the error bars. The lowest-frequency bin has the largest error bar. The next two bins are roughly consistent with the input lag and have an error-weighted mean of −48 days. Because there is no short lag and it is at frequencies higher than the wrapping frequency (vertical gray line), the highest-frequency bin is consistent with zero.
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 cross-correlation coefficients of even daily cadence light curves that have been reprocessed with long (short) lags of −50 (7), −130 (9), and −400 (12) days, in the top, center, and bottom panels, respectively. Distributions shown in orange have been reprocessed with only a long lag. The ratios of the amplitude of the long to the amplitude of the short lag for the light curves with distributions shown in green, light blue, and pink, are 0.2, 0.1, and 0.01, respectively. The dashed vertical lines show the input lags.
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 mean of the Von-Neumann value or the mean-square successive-difference for 1000 MCMCs as a function of lag for three mock long season LSST light curves with input long lags of −50, −130, and −400 days and short lags of 7, 9, and 12 days in the top, middle, and bottom panels, respectively. The ratios of the amplitude of the long lag to the amplitude of the short lag are 0.2 (left panels), 0.1 (middle panels), and 0.01 (right panels). The dashed vertical lines show the input lags.
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 leftmost panel shows the rest-frame short lag between the u and y band in days calculated using the standard thin-disk model, and the remaining panels show the long lag timescale between the u and y band in days for disks with aspect ratios from left to right of 0.03, 0.1, and 0.3 as a function of Eddington ratio and SMBH mass in M ☉. The white point shows the approximate SMBH mass and Eddington ratio of Fairall 9 (Peterson et al. 2004; Hernández Santisteban et al. 2020).
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: An example JAVELIN distribution for a mock light curve with the baseline cadence. While there is a very small peak around the input lag (shown as a dashed line) of −50 days, the peaks around ±180 days are larger.
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: Overall evolution of the event. (a) Photospheric magnetogram of the selected cube at t = 0 s. P1 and N1 mark two strong and coherent sunspots, and P2 and N2 mark two weak and diffuse sunspots. (b) A zoomed-in view of main magnetic structures in the corona at t = 0 s. The twisted magnetic flux rope anchored in P1 and N1 is marked in purple. The golden lines outline three groups of magnetic arcades in the lower corona (LA-1, LA-2, and LA-3), while the HAs are marked in dark green. (c)–(e) Evolution of the flux rope before and during the confined eruption. The colors of magnetic field lines follow those in (b). The white lines in (c) mark the boundaries of the selected vertical planes within which we average the parameters to yield a 2D slice. The red, light green, and blue arrows indicate the x-, y-, and z-axis, respectively. The 3D visualization is produced by VAPOR (Li et al. 2019). (f)–(h) Synthetic AIA 171 Å and XRT Al-thick images from side views during the same times as (c)–(e).
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: Kinematic evolution of the flux rope. (a) Height–time diagram of plasma density along slit S1, where the upper edge of the flux rope is marked by white crosses. The insert shows the position of S1 (white line) on the averaged 2D plasma density map. (b) The measured height of the flux rope fitted with a curve following the function marked at the top (b). (c) Velocity of the flux rope derived from the time derivative of the measured height. The red line shows the GOES 1–8 Å flux. For comparison, the blue line shows the time derivative of the fitting function shown in (b). (d) Acceleration of the flux rope derived from the time derivative of the velocity. The black crosses in (b)–(d) indicate the data points used for curve fitting, while the excluded data are shown in gray. The green dashed lines in (b)–(d) indicate the observational onset time t  b .
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: The magnetic field and decay index along the trajectory of the flux rope. (a) Distribution of the external poloidal field (green curve) and the external toroidal field (yellow curve) vs. height along the eruption trajectory S1 on a sampled slice. The ratio of the external poloidal field to the horizontal component of the potential field is shown as the gray curve. (b) Distribution of the mean decay index vs. height, which is averaged over the sampled positions of the flux rope. The gray dotted and dashed lines indicate the value of the decay index at 1.0 and 1.5, respectively. The positions of the upper edge and the axis of the flux rope at t  b  are marked with blue and red vertical dashed lines, respectively.
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: Dynamic behaviors and reconnection characteristics during the eruption. (a) Distribution of the Lorentz force (red), the gas pressure gradient (orange), the gravity (blue), and the net force (black) along S1 at t = 704.03 s. (b) Distribution of temperature (red) and plasma density (blue) along S1 at t = 704.03 s. (c) Map of v  z  on an x–z plane located at y = 48.96 Mm at t = 704.03 s. Magnetic field lines corresponding to the flux rope (blue), the newly reconnected arcades (green), and the post-flare loops (red) are projected in the plane. The black dashed lines in (a) and (b) mark the upper boundary of the flux rope calculated by Equations (1), and the gray dashed lines in (a)–(c) mark the position of the maximum Lorentz force.
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: Force and acceleration within the flux rope during the slow-rise phase. (a) Main force terms averaged over the flux rope region. The red, blue, and orange curves indicate the Lorentz force, gravity, and gas pressure gradient, respectively. The black curve marks the evolution of the net force. (b) The corresponding accelerations calculated by dividing each force by the mass of the flux rope, which are plotted in the same colors as that in (a). The green dashed lines indicate the observational onset time t  b .
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 long lags (left panel) and short lags (right panel) recovered by the maximum-likelihood method for light curves that have not been reprocessed with a lag for all cadences in the paper. From top to bottom, the light curves have been subsampled with the long season LSST u- and y-band cadence, the baseline u- and y-band cadence, the baseline g- and z-band cadence, and the baseline g- and z-band cadence + LCO 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: The top panel shows the lags recovered by JAVELIN, and the bottom panel shows the lags recovered by the maximum-likelihood method for 16 mock light curves made from the simulation in Jiang & Blaes (2020) with no input lag and the long season LSST 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: Eight individual JAVELIN distributions for light curves with no reprocessing and the long season LSST cadence. Each panel is labeled with the median of the positive and negative values of the distribution.
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: Synthetic transmission spectra of warm exoplanets. The left panel shows the transit depths of Jupiter-mass planets orbiting around a Sun-like star with various equilibrium temperatures, where we assume 1 Gyr age. The black lines show the spectra without NH3 and HCN, and the blue and orange shaded parts denote the excess transit depth when we include NH3 and HCN absorption. The upper right panel shows the spectra of Jupiter-mass planets with T eq = 800 K at different system ages. The lower right panel shows the spectra for sub-Jupiter (M p = 0.11 M J) and Jupiter mass (1 M J) planets with T eq = 800 K at 1 Gyr age. We assume solar composition atmospheres and K zz = 108 cm2 s−1 for all spectra shown here.
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: (Top) Stellar spectra λ F  λ  at the stellar surface. The yellow, magenta, and navy lines show the spectra of G-type (Sun), K-type (HD 40307), and M-type (GJ 1214) stars, respectively. The flux is normalized by the maximum value. The gray-shaded region denotes the wavelength band of 200–230 nm, which mainly drives NH3 photodissociation. (Bottom) Vertical distributions of NH3 (solid lines) and HCN (dashed lines) on warm planets around the different spectral type stars listed in the top panel. We assume a Jupiter-mass planet with age of 1 Gyr, T eq = 600 K, and K zz = 108 cm2 s−1.
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: Strength of NH3 (top row) and HCN (bottom row) absorption features as a function of wavelength and planetary equilibrium temperature (see Section 4.3 for the definition of the feature strength). The left and right columns show the results for transmission and emission spectra, respectively. The black, gray, and silver lines denote the contours of 50, 100, and 300 ppm, respectively. The colored arrows at the bottom of each panel denote the wavelength range of JWST NIRISS (0.6–2.8 μm), NIRCam (2.5–5 μm), NIRSpec (0.7–5 μm), and MIRI (5–14 μm), taken from Batalha et al. (2017). We have assumed a Jupiter-mass planet around a Sun-like star at 1 Gyr age with a solar composition atmosphere and K zz = 108 cm2 s−1.
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: Synthetic emission spectra of giant planets around a Sun-like star. The black lines show the spectra without NH3 and HCN, and the blue and orange shaded parts denote the reduction of planetary thermal emission when we include NH3 and HCN absorption. The left panel shows the spectra of Jupiter-mass planets at 1 Gyr age for various planetary equilibrium temperatures. The right top three panels show the spectra of Jupiter-mass planets with T eq = 800 K at different ages. The bottom right panel shows the spectra for T eq = 800 K and 1 Gyr age at different planetary masses. We have assumed solar composition atmospheres and K zz = 108 cm2 s−1 for all spectra presented here.
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: Vertical distributions of NH3 and HCN for different parameterizations of K zz. The blue and orange dashed–dotted, solid, dashed lines show the vertical distribution of NH3 and HCN for vertically varying K zz with K zz,1 bar = 106, 108, and 1010 cm2 s−1, respectively. The green solid and dotted lines show the distributions for vertically constant K zz = 108 cm2 s−1 for reference. We have assumed a Jupiter mass planet with a solar composition atmosphere, T eq = 800 K, and 1 Gyr age.