adsabs/AstroCLIMB huggingface dataset:
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: 90% completeness estimate based on cross-referencing spectroscopically identified stars with the catalog by Trippe et al. (2008).
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Hierarchical likelihood for an injected n  L  = 106 Mpc−3 density, with ∼200 gravitational-wave events. The likelihood correctly recovers the injected hyperparameter 106 Mpc−3, with 95% CI intervals of 105.1 and 106.5 Mpc−3, and so is capable of not only constraining the population properties of IMBHs but actually detecting them.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Corner plot posterior for an injection with ﹩{\mathrm{log}}_{10}(y)\sim -0.05﹩ and ﹩{\mathrm{log}}_{10}({M}_{{Lz}})\sim 4﹩, with the gold lines demarcating the injected values of ﹩({M}_{{Lz}},y,{d}_{L},{{ \mathcal M }}_{C})﹩. Both the injected M  Lz  and y values are recovered with reasonable precision, and their distributions are approximately normal. Inclusion of the lens parameters does not significantly bias the source luminosity distance d  L  or chirp mass ﹩{{ \mathcal M }}_{C}﹩.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption:  πΣ(z  S , n  L  = 1000 Mpc−3) as a function of source redshift, comparing the analytical spatial Poisson model (orange) to simulated, fitted values (blue). As Σ increases monotonically with source redshift, π(y∣z  S , n  L ) shifts toward smaller y. Thus, detector networks with a larger detectable range are more likely to detect lensed sources.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Hierarchical likelihood for an injected n  L  = 103 Mpc−3 density, with ∼200 gravitational-wave events. At 95% CI, the density is constrained to ≲104.6 Mpc−3. Further detections of gravitational waves unlensed by IMBHs could push this constraint further down, as well as an expanded, more sensitive detector network.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Corner plot with an injected y ≫ 1 in ﹩\{{M}_{{Lz}},y,{d}_{L},{{ \mathcal M }}_{C}\}﹩, with the injected values marked by the gold lines. In contrast to the small y case, at large y the lens-mass posterior is completely agnostic, as is the M  Lz  posterior.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Orbits and astrometric measurements of the 36 young stars in the Galactic Center. The track of astrometric measurements is overplotted as darkened points. The orbits of the young stars belonging to the clockwise disk are shown. The inset shows the “Sgr A* star cluster” of the innermost young stars, which are on preferentially eccentric and randomly distributed orbits.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Peak π(y∣z  S ) value as a function of z  S . The y distribution shifts toward smaller values as the effective lens surface density grows.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Like Figure 5 for the central arcsecond, plotted in linear scale. The color scale is truncated at 10σ pixle, which corresponds to a p-value of ∼99%.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Lookup map of young stars without accelerations: young stars used in this study. The number indicated next to the star corresponds to the row index in column # in Table 5.
Paper: Inferring the Intermediate-mass Black Hole Number Density from Gravitational-wave Lensing Statistics
Authors: Joseph Gais, Ken K. Y. Ng, Eungwang Seo, Kaze W. K. Wong, Tjonnie G. F. Li
Figure caption: Corner plot of (y, z  L , M  L ) distributions simulated directly (blue), without bias factor (dashed black line), and with bias factor (orange), for α  L  = 1. Because of the lensing bias from selecting source–lens pairs with the smallest y value, the selected lens-mass and lens-redshift distributions, ﹩{\pi }_{{z}_{L}}\left({z}_{L}| {z}_{S},{{\boldsymbol{\Lambda }}}_{L},{ \mathcal P }\right){\pi }_{{M}_{L}}\left({M}_{L}| {z}_{S},{{\boldsymbol{\Lambda }}}_{L},{ \mathcal P }\right)﹩, are different from their preselection distribution, ﹩{\pi }_{{z}_{L}}^{{\prime} }\left({z}_{L}| {z}_{S},{{\boldsymbol{\Lambda }}}_{L}\right){\pi }_{{M}_{L}}^{{\prime} }\left({M}_{L}| {z}_{S},{{\boldsymbol{\Lambda }}}_{L}\right)﹩, and direct simulations confirm our bias factor. After selection, the lens-redshift distribution now scales as ﹩\displaystyle \frac{{D}_{{LS}}}{{D}_{L}}\tfrac{{{dV}}_{c}}{{{dz}}_{L}}﹩, and ﹩{\pi }_{{M}_{L}}\left({M}_{L}| {z}_{S},{{\boldsymbol{\Lambda }}}_{L},{ \mathcal P }\right)﹩ is uniform. Furthermore, independent sampling of (y, z  L , M  L ; orange contours) align with the direct simulation contours (blue), and so the 1D distributions are indeed uncorrelated following selection of minimum y.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Significance (σ pixel) of the overdensity of the angular momentum distribution in logarithmic scale as a function of projected radius slice, computed using the isotropic cluster prior. See text for details.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Left to right: the determinant of the Jacobian (﹩| \det (\mathrm{Jac})| ﹩), orbital element probability distribution function (PDFiso−clus.), and coordinate-transformed probability distribution function (﹩\mathrm{PDF}{{\prime} }_{\mathrm{iso}-\mathrm{clus}.}﹩) of the star IRS 34W as a function of z distance. The transformed ﹩\mathrm{PDF}{{\prime} }_{\mathrm{iso}-\mathrm{clus}.}﹩ is the product of the determinant and the isotropic cluster PDF. Note that the y-axis for each plot is different.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: KLFs of stars associated with the different kinematic features and the KLF of all young stars including the central S stars. No explicit projected radius cut is applied, but we combine the stars of clockwise disk (CW1 and CW2).
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Comparison of stars belonging to the CW1 (green) and CW2 (blue) disks. Stars that do not belong to either feature are plotted in gray. The inset shows the prior width and direction of the feature prior L feat based on which the colored stars are selected (i.e., Δ log evidence >2, Section 5). Stars marked with a “plus” have positive radial velocity, unmarked stars have a negative radial velocity. The arrows indicate the direction of the projected velocity. In both cases we evaluate the disk membership probability for all young stars, i.e., no radial binning has been applied.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Significance (σ pixel) of the overdensity of angular momentum for stars at a projected distance from 4″ to 8″. The figure is identical to the bottom-leftmost panel of Figure 4, however the color scaling is adapted and in linear scale.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Distribution of the eccentricity and the semimajor axis of the stars consistent with belonging to the inner part of the warped clockwise disk. The dark green histograms show the properties of the 5D-constrained stars, and the light green histogram show the distribution of stars with determined orbital solutions. The gray and black vertical lines indicate the median, and the dashed lines indicate the IQR of the stars with and without orbit.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Illustration of the location and width of the feature priors assumed, tabulated in Table 1.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Same as Figure 9 for CCW/F1 (purple), F2 (pink), and F3 (orange).
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Same as Figure 5, projected distance from 8″ to 16″, again with adapted color scaling and in linear scale.
Paper: Kink Oscillation of a Flux Rope During a Failed Solar Eruption
Authors: Pankaj Kumar, Valery M. Nakariakov, Judith T. Karpen, C. Richard DeVore, Kyung-Suk Cho
Figure caption: (a), (c), (e), and (g) Waveforms extracted from the TD plots in Figures 2 and 3 (slits S1 to S3). The blue dashed curves show the parabolic trends subtracted to produce the detrended waveforms in panels (b), (d), (f), and (h). The blue and red curves are best-fit exponentially decaying sine functions. The start time for each panel is 15:13:49 UT.
Paper: Kink Oscillation of a Flux Rope During a Failed Solar Eruption
Authors: Pankaj Kumar, Valery M. Nakariakov, Judith T. Karpen, C. Richard DeVore, Kyung-Suk Cho
Figure caption: (a) and (c) SDO/AIA 171 Å images at two times during the failed eruption, showing the locations of slits S1 and S2 used to construct the TD intensity plots in panels (b) and (d), which display the kink oscillations of the FR. Arrows in (d) indicate the overlying loops. In panel (a), L1 and L2 mark the two legs of the flux rope.
Paper: Kink Oscillation of a Flux Rope During a Failed Solar Eruption
Authors: Pankaj Kumar, Valery M. Nakariakov, Judith T. Karpen, C. Richard DeVore, Kyung-Suk Cho
Figure caption: (a) SDO/HMI magnetogram showing ARs 12017 and 12018 on 2014 March 30. Red/blue shading indicates positive/negative polarities (contour levels = ±100 G). Filament eruption occurred in AR 12018 (marked by yellow ellipse). (b) Potential-field extrapolation of the ARs (same field of view as shown in panel (a)). Red field lines are arcades overlying the erupting AR 12018 (cyan). Open field lines are shown in green. Yellow field lines represent connecting loops in the neighboring AR 12017.
Paper: Kink Oscillation of a Flux Rope During a Failed Solar Eruption
Authors: Pankaj Kumar, Valery M. Nakariakov, Judith T. Karpen, C. Richard DeVore, Kyung-Suk Cho
Figure caption: DEM maps of the FR in different temperature bins using six nearly simultaneous AIA images around 15:19:37 UT. The field of view is the same as in Figures 2 and 3.
Paper: GB6 J2113+1121: A Multiwavelength Flaring γ-Ray Blazar Temporally and Spatially Coincident with the Neutrino Event IceCube-191001A
Authors: Neng-Hui Liao, Zhen-Feng Sheng, Ning Jiang, Yu-Ling Chang, Yi-Bo Wang, Dong-Lian Xu, Xin-Wen Shu, Yi-Zhong Fan, Ting-Gui Wang
Figure caption: Upper panels: smoothed γ-ray test static (TS) maps (10° × 10° scale with 0.°2 per pixel; GB6 J2113+1121 not included in the mode file) of the region that is spatially compatible with the arrival direction of the neutrino IC 191001A. The left one is based on the Fermi-LAT data with a time range between MJD 54,683 (i.e., the beginning of its operation) and MJD 58,383 (marked as a black vertical dashed line in the bottom panel), while the right one corresponds to the rest of the Fermi-LAT data. The black circle represents the 95% C. L. γ-ray localization error radius of GB6 J2113+1121, and the black cross corresponds to its radio location. Bottom panel: half-year time bin γ-ray light curves of the three γ-ray sources spatially coincident with the neutrino IC 191001A. Blue circles and red triangles are flux estimations and upper limits, and TS values corresponding to each time bin are also shown. The horizontal lines represent the averaged fluxes of the sources for the entire data set along with the 1σ uncertainties. The red vertical line marks the arrival time of the neutrino IC 191001A.
Paper: Discrepancy between the Low-frequency Cutoffs of Type III Radio Bursts Based on Simultaneous Observations by WIND and PSP
Authors: Bing Ma, 兵 马, Ling Chen, 玲 陈, Dejin Wu, 德金 吴, Marc Pulupa, Stuart D. Bale
Figure caption: Comparison of observations by PSP and WIND when the minimum azimuth difference Δθ < 30° in the two cases of PSP near orbital perihelion and aphelion. Panel (a) shows the positions of Earth (or WIND) and PSP when PSP approaches the perihelion on 2019 April 6. The corresponding dynamic spectra observed by PSP and WIND at 07:30–12:00 UT on this day are shown in panels (c) and (e), respectively. In contrast, panels (b), (d), and (f) show the case of PSP near its aphelion on 2020 July 21, and the corresponding dynamic spectra observed by PSP and WIND at 01:00–08:30 UT, respectively.
Paper: Discrepancy between the Low-frequency Cutoffs of Type III Radio Bursts Based on Simultaneous Observations by WIND and PSP
Authors: Bing Ma, 兵 马, Ling Chen, 玲 陈, Dejin Wu, 德金 吴, Marc Pulupa, Stuart D. Bale
Figure caption: Two examples of edge recognition using the Canny method for type III bursts. The radio dynamic spectra of WIND/WAVES and PSP/RFS are shown in panels (a) and (b), respectively. The blue dots or lines are the edges of type III bursts and other noises obtained by the Canny method. In each panel, the lowest point in the edge of a clear type III burst is marked by a yellow point, and the corresponding cutoff frequency f  lo  is labeled by the red dashed line.
Paper: Discrepancy between the Low-frequency Cutoffs of Type III Radio Bursts Based on Simultaneous Observations by WIND and PSP
Authors: Bing Ma, 兵 马, Ling Chen, 玲 陈, Dejin Wu, 德金 吴, Marc Pulupa, Stuart D. Bale
Figure caption: The histogram of the characteristic frequency (f  lo  and f  p ) of type III bursts observed during the time from 2019 January 1 to 2020 July 31. Panels (a) and (b) show the 491 and 1194 type III events observed by WIND and PSP, respectively.
Paper: Discrepancy between the Low-frequency Cutoffs of Type III Radio Bursts Based on Simultaneous Observations by WIND and PSP
Authors: Bing Ma, 兵 马, Ling Chen, 玲 陈, Dejin Wu, 德金 吴, Marc Pulupa, Stuart D. Bale
Figure caption: The minimum azimuth difference Δθ between WIND and PSP in the HGI coordinate. The curve marked by the green circles shows all the angles of minimum azimuth difference from 2019 January 1 to 2020 July 31 in a temporal resolution of 1 day. Blue squares label the dates when PSP is in the encounter phases. The red solid line represents the position where Δθ equals 30°.
Paper: GB6 J2113+1121: A Multiwavelength Flaring γ-Ray Blazar Temporally and Spatially Coincident with the Neutrino Event IceCube-191001A
Authors: Neng-Hui Liao, Zhen-Feng Sheng, Ning Jiang, Yu-Ling Chang, Yi-Bo Wang, Dong-Lian Xu, Xin-Wen Shu, Yi-Zhong Fan, Ting-Gui Wang
Figure caption: Multiwavelength light curves of GB6 J2113+1121. In the monthly γ-ray light-curve panel, the horizontal and black dashed vertical lines are the same as those in Figure 1. For the Swift-UVOT measurements, corrections of the Galactic absorption have been carried out (Cardelli et al. 1989; Schlafly & Finkbeiner 2011). For the ZTF light curves, the solid markers represent the magnitudes of the target, while the hollow ones correspond to average values of the comparison stars in the same field. The red vertical line across all panels marks the arrival time of the neutrino.
Paper: GB6 J2113+1121: A Multiwavelength Flaring γ-Ray Blazar Temporally and Spatially Coincident with the Neutrino Event IceCube-191001A
Authors: Neng-Hui Liao, Zhen-Feng Sheng, Ning Jiang, Yu-Ling Chang, Yi-Bo Wang, Dong-Lian Xu, Xin-Wen Shu, Yi-Zhong Fan, Ting-Gui Wang
Figure caption: Comparisons between GB6 J2113+1121 and 4LAC blazars (Ajello et al. 2020), in which the known neutrino-emitting blazar candidates are highlighted. The energy ranges corresponding to the energy flux and the photon flux are between 100 MeV and 100 GeV. In the right panel, the 4LAC values of the candidates are colored in yellow; meanwhile, values corresponding to the flares temporally coincident with the arrival of neutrinos (Kadler et al. 2016; IceCube Collaboration et al. 2018a; Garrappa et al. 2019b; Franckowiak et al. 2020) are plotted in blue. For PKS B1424-418, no available spectral information in the high-flux state is found.
Paper: GB6 J2113+1121: A Multiwavelength Flaring γ-Ray Blazar Temporally and Spatially Coincident with the Neutrino Event IceCube-191001A
Authors: Neng-Hui Liao, Zhen-Feng Sheng, Ning Jiang, Yu-Ling Chang, Yi-Bo Wang, Dong-Lian Xu, Xin-Wen Shu, Yi-Zhong Fan, Ting-Gui Wang
Figure caption: The broadband SED of GB6 J2113+1121. Simultaneous data are colored. The blue ones represent the high-flux state and the red ones correspond to the low-flux state. The 1 yr averaged γ-ray spectrum corresponding to the long-term high-flux state is plotted in cyan symbols. Multiwavelength data of GB6 J2113+1121 that are strictly simultaneous with the neutrino arrival are also plotted (in yellow). Nonsimultaneous data are in gray.
Paper: GB6 J2113+1121: A Multiwavelength Flaring γ-Ray Blazar Temporally and Spatially Coincident with the Neutrino Event IceCube-191001A
Authors: Neng-Hui Liao, Zhen-Feng Sheng, Ning Jiang, Yu-Ling Chang, Yi-Bo Wang, Dong-Lian Xu, Xin-Wen Shu, Yi-Zhong Fan, Ting-Gui Wang
Figure caption: P200 spectrum. The spectrum is plotted in black and smoothed by a window with a length of 16 Å, while the uncertainty is in orange. The vertical dotted lines mark the main emission lines. The blue shaded regions represent the position of the dichroic or the uncorrected telluric.
Paper: A New Method for Measuring Infrared Band Strengths in H2O Ices: First Results for OCS, H2S, and SO2 
Authors: Yukiko Y. Yarnall, Reggie L. Hudson
Figure caption: IR measurements for H2O+X ices (X = OCS, H2S, and SO2), with three H2O:X ratios in each case and all spectra recorded at 10 K. Ice thicknesses ranged from about 0.2 to 1.2 μm.
Paper: Radical Recombination during the Phase Transition of Interstellar CO Ice
Authors: Jiao He, Sándor Góbi, Gopi Ragupathy, György Tarczay, Thomas Henning
Figure caption: RAIRS spectra of (a) CO, (b) 13CO, (c) CH3OH, (d) HCO, (e) H2CO, and CO2 after deposition at 3.1 K, after UV irradiation at 3.1 K, and at a few selected temperatures (4.2, 4.7, 5.3, 28.1, and 39.3 K) during the subsequent linear warm-up (TPD).
Paper: A New Method for Measuring Infrared Band Strengths in H2O Ices: First Results for OCS, H2S, and SO2 
Authors: Yukiko Y. Yarnall, Reggie L. Hudson
Figure caption: From top to bottom, IR spectra of amorphous ices at 10 K made from H2O+OCS, H2O+H2S, and H2O+SO2, each with a mixing ratio of ∼10:1 and a thickness of ∼1 μm. Spectra are offset vertically for clarity. The broad IR bands near 3300, 2200, 1650, and 800 cm−1 are from H2O ice.
Paper: Radical Recombination during the Phase Transition of Interstellar CO Ice
Authors: Jiao He, Sándor Góbi, Gopi Ragupathy, György Tarczay, Thomas Henning
Figure caption: RAIRS spectra of the CH3OH:CO = 7.1:100 mixed ice: (1) after deposition at 3.1 K, (2) after 30 minutes of UV irradiation at 3.1 K, (3) during the warm-up at 5.3 K, and (4) during the warm-up at 40.2 K. The three newly formed major species, HCO, H2CO, and CO2, are labeled in the figure.
Paper: Radical Recombination during the Phase Transition of Interstellar CO Ice
Authors: Jiao He, Sándor Góbi, Gopi Ragupathy, György Tarczay, Thomas Henning
Figure caption: Band area of the HCO and H2CO absorption peaks at ∼1854 and ∼1720 cm−1, respectively, during the warm-up of the UV-processed CH3OH:CO=7.1:100 mixed ice.
Paper: Radical Recombination during the Phase Transition of Interstellar CO Ice
Authors: Jiao He, Sándor Góbi, Gopi Ragupathy, György Tarczay, Thomas Henning
Figure caption: RAIRS spectra of CH3OH:CO = 7.1:100 mixed ice between 1110 and 1300 cm−1: (1) after deposition at 3.1 K; (2) after 30 minutes of UV irradiation at 3.1 K; and (3) during the warm-up (TPD) at 4.2, 4.7, and 5.3 K. The expected position of CH2OH absorption is marked.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Corner plot of the MCMC posterior sample density distributions. Orange histograms and contours show the results for the wide χ e prior, while the blue ones are for the narrow prior. The black dashed lines in the plots on the diagonal bracket the 1σ credible interval, while the red solid lines mark the position of the estimated best fit.