adsabs/AstroCLIMB huggingface dataset:
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Left: white light curve for the transit of K2-18 b observed with NIRSpec 							G395H. The top panel shows the combined white light curve from NRS1 and 							NRS2, together with the 1σ model interval 							in red. The bottom panel shows the residuals after subtracting the 							median model, together with the line at zero. The standard deviation of 							the residuals is measured to be 123 ppm, which is 1.2× the expected 							noise level. The red line is shown to indicate zero. Right: the top 							panel shows the normalized spectroscopic light curves (binned in 							wavelength for visual clarity). The detector gap is shown in white. The 							bottom panel depicts the transit depth precision at pixel 							resolution.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Spectral contributions of key molecular species in the 1–5 μm range. The different curves show individual 							contributions from different molecules to a nominal model transmission 							spectrum of K2-18 b shown in black and denoted as “Combined.” The model 							assumes a mixing ratio of 10−2 for CH4 and 								CO2, 10−4 for H2O, and 								10−5 for all the other species, consistent with our 							retrieval estimates discussed in Section 3, and an isothermal temperature profile 							of 250 K. Each curve corresponds to a transmission spectrum with opacity 							contributions from a single molecule at a time, in addition to 								H2–H2 and H2–He collision-induced 							absorption. The spectral ranges of our JWST NIRISS and NIRSpec 							observations are also indicated; the NIRSpec range spans two detectors 							(NRS1 and NRS2), with a gap between them spanning 3.72-3.82 μm.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Retrieved spectral fit of the JWST transmission spectrum of K2-18 b using 							a model without clouds/hazes in the one-offset case. Details of the 							figure are the same as for Figure 3, except that the retrieval does not 							include clouds/hazes in the model. The retrieval produces a comparable 							fit to the cloudy case (Figure 3) across most of the wavelength range, differing mostly 							toward the bluer end of the NIRISS band, as discussed in Appendix B. The NIRSpec spectrum 							is vertically offset by -30 ppm, corresponding to the median retrieved 							offset.
Paper: Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
Authors: S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua
Figure caption: Example spectra from two ICMEs. From top to bottom, the panels show the trace PSD with power-law fits in the inertial and transition ranges, magnetic compressibility spectrum, and spectral index of the trace PSD. Vertical lines mark spacecraft-frame frequencies associated with the spectral break point, f b, the k ρ i = 1 scale, ﹩{f}_{{\rho }_{{\rm{i}}}}﹩, and the kd i = 1 scale, ﹩{f}_{{d}_{{\rm{i}}}}﹩. Horizontal lines in the bottom panels mark characteristic α values (−1, −5/3, and −2.8).
Paper: Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
Authors: S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua
Figure caption: Ratios of f b to ﹩{f}_{{d}_{{\rm{i}}}}﹩ and ﹩{f}_{{\rho }_{{\rm{i}}}}﹩ as a function of β i with five-point running average lines (top panel), smoothed compressibility spectra (middle panel), and mean spectral index (bottom panel) with characteristic values (−1, −3/2, −5/3, and −2.8) marked by horizontal lines.
Paper: Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
Authors: S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua
Figure caption: Radial evolution of magnetic field parameters within the ICME intervals, color-coded to β i. From top to bottom, the panels show the integrated fluctuation power, fluctuation amplitude normalized to the mean field strength, compressibility, inertial-range spectral index, spectral break frequency, and mean-subtracted correlation length. Gray lines show five-point moving averages and black dashed lines show power-law fits as a function of r.
Paper: Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
Authors: S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua
Figure caption: Low-frequency analysis. The top left panel shows the magnetic field time series for an example ICME, overlaid with dashed–dotted lines indicating the component mean values and solid lines showing a GH fit. Vertical lines mark the ICME boundaries. The right panel shows trace PSDs of the mean-subtracted, GH-subtracted, and modeled GH flux rope field. The bottom left panel shows λ, λ M, and λ GH vs. ICME radial width, L, with five-point running averages shown by the smooth lines and y = x by the dashed line.
Paper: Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
Authors: S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua
Figure caption: Smoothed, trace PSD of magnetic field fluctuations for a selection of the ICMEs analyzed. Red points mark spectral break frequencies.
Paper: A Single Ejection Model of the DART/Dimorphos Debris Trail
Authors: Yoonyoung Kim, David Jewitt
Figure caption: Scattering cross section of the debris trail within a 50 km radius projected aperture as a function of time. The solid black line shows an exponential fit to the data. The secondary tail ejection time from the model of Li et al. (2023) is indicated.
Paper: A Single Ejection Model of the DART/Dimorphos Debris Trail
Authors: Yoonyoung Kim, David Jewitt
Figure caption: The surface brightness vs. distance along the trail (black line; 0.001 = 27.2 mag arcsec−2). Lines show models for a power law, broken at a = 1 cm, with differential indices q = 3.9 and 4.0 (green), q = 3.9 and 4.2 (blue), and q = 3.9 and 4.4 (magenta). Approximate locations of particles as a function of their radius are marked. The nucleus was saturated in the data and was not fitted.
Paper: A Single Ejection Model of the DART/Dimorphos Debris Trail
Authors: Yoonyoung Kim, David Jewitt
Figure caption: Composite HST image from UT 2023 February 4, rotated so that the trail lies horizontally. We mark the distances reached by dust particles under the action of radiation pressure, as a function of their radius (in centimeters).
Paper: Quasiperiodic Peak Energy Oscillations in X-Ray Bursts from SGR J1935+2154
Authors: Oliver J. Roberts, Matthew G. Baring, Daniela Huppenkothen, Chryssa Kouveliotou, Ersin Göğüş, Yuki Kaneko, Lin Lin, Alexander J. van der Horst, George Younes
Figure caption: Left: light curves of bursts 1 (bn220116590) and 2 (bn22012832) plotted alongside each other within a 500 ms window starting at –130 ms. The trigger time for each event is the zero time. The first, weaker emission episode in burst 1 lasts about 100 ms, starting at ∼125 ms. Middle: ∼175 ms window showing the E  p  behavior of bursts 1 (pink) and 2 (purple). Burst 1 is shifted in time by –166 ms in order to show the similar E  p  oscillating frequency of 24 ms (42 Hz), highlighted by the dashed gray lines. Right: correlation between the energy flux (﹩{ \mathcal F }﹩) and peak energy (E  p ) of ﹩{ \mathcal F }\,\propto \,{E}_{{p}}^{3.2\pm 0.2}﹩, identified using data from both bursts The temporal binning for all panels is 4 ms.
Paper: Quasiperiodic Peak Energy Oscillations in X-Ray Bursts from SGR J1935+2154
Authors: Oliver J. Roberts, Matthew G. Baring, Daniela Huppenkothen, Chryssa Kouveliotou, Ersin Göğüş, Yuki Kaneko, Lin Lin, Alexander J. van der Horst, George Younes
Figure caption: Searching for (quasi-)periodicities in E  p  with a Gaussian process–based model in burst 1. Left: E  p  values with uncertainties (black) as a function of time, along with posterior draws of the skew-Gaussian mean function (green) and the combined model of skew-Gaussian and DRW (orange). Overall, this model, containing only aperiodic stochastic variability on top of the overall skew-Gaussian trend, fits the E  p  very well. Middle: same as the left panel but for a model where the DRW was replaced by a QPSO parameterized as a stochastically driven, damped harmonic oscillator. This model also describes the data adequately well. The resulting Bayes factor does not allow us to favor one model over the other. Right: posterior probability density for the period of the QPSO in the model shown in the middle panel, showing that the time series constrains the QPSO period well.
Paper: Quasiperiodic Peak Energy Oscillations in X-Ray Bursts from SGR J1935+2154
Authors: Oliver J. Roberts, Matthew G. Baring, Daniela Huppenkothen, Chryssa Kouveliotou, Ersin Göğüş, Yuki Kaneko, Lin Lin, Alexander J. van der Horst, George Younes
Figure caption: Searching for (quasi)periodicities in the flux light curve for burst 1 with a Gaussian process–based model. Left: flux (in units of counts per second) values with uncertainties (black) as a function of time, along with posterior draws of a mean function parameterized as a superposition of three skew-Gaussian functions (green) and the combined model of skew-Gaussian mean function and DRW covariance function (orange). Middle: same as the left panel but for a model where the DRW covariance was replaced by a QPO, parameterized as a stochastically driven, damped harmonic oscillator. We find that the Bayes factor strongly prefers the red-noise model over the QPO model. Right: posterior probability density for the period of the QPO in the model shown in the middle panel. The posterior is broad and covers much of the available prior range.
Paper: A Single Ejection Model of the DART/Dimorphos Debris Trail
Authors: Yoonyoung Kim, David Jewitt
Figure caption: Comparison between HST images (left) and Monte Carlo models (right). A linear scale bar, the projected antisolar direction (−S), and the negative heliocentric velocity vector (−V) are indicated. The Dimorphos location is marked with a cross in each panel. Note the scale change in the last row of panels.
Paper: A Single Ejection Model of the DART/Dimorphos Debris Trail
Authors: Yoonyoung Kim, David Jewitt
Figure caption: Viewing angle (angle between the trail axis and the line of sight) as a function of time, expressed as days after impact. The shaded region indicates when the double tail was observed. The ejecta cone is viewed edge-on when viewing angle = 90° (dashed line), at which point the walls of the hollow cone are most clearly visible.
Paper: One, Two, Three ... An Explosive Outflow in IRAS 12326-6245 Revealed by ALMA
Authors: Luis A. Zapata, Manuel Fernández-López, Silvia Leurini, Estrella Guzmán Ccolque, I. M. Skretas, Luis F. Rodríguez, Aina Palau, Karl M. Menten, Friedrich Wyrowski
Figure caption: Position−radial velocity diagram of the explosive streamers detected in IRAS12326−6245 with our ALMA observations. The most southern and farther filament shown in Figure 1 is not plotted here for convenience. We have plotted the blueshifted streamers in blue colors, while the redshifted ones in red. All the molecular streamers are mostly pointing to some place around a radial velocity to −39.5 km s−1, the systemic cloud velocity of IRAS12326−6245. In position, the center is located at α  J2000.0 = 12h35m35s147, and δ  J2000.0 = 63°02′30.″48. In each filament the shaded or blurry blue and red colors represent the error area that is about 0.″1 for the on-the-sky distance.
Paper: One, Two, Three ... An Explosive Outflow in IRAS 12326-6245 Revealed by ALMA
Authors: Luis A. Zapata, Manuel Fernández-López, Silvia Leurini, Estrella Guzmán Ccolque, I. M. Skretas, Luis F. Rodríguez, Aina Palau, Karl M. Menten, Friedrich Wyrowski
Figure caption: ALMA moment one (color-scale image) overlaid with the positions/radial velocities of the CO(2−1) condensations (color dots) from the most southern redshifted explosive molecular filament (see Figure 1). The filament and the condensations show a clear velocity gradient, with the most redshifted velocities localized far from its origin, i.e., showing Hubble–Lemaitre–like expansion motions. This velocity trend has been observed in other explosive molecular streamers; see, for an example, Zapata et al. (2017).
Paper: One, Two, Three ... An Explosive Outflow in IRAS 12326-6245 Revealed by ALMA
Authors: Luis A. Zapata, Manuel Fernández-López, Silvia Leurini, Estrella Guzmán Ccolque, I. M. Skretas, Luis F. Rodríguez, Aina Palau, Karl M. Menten, Friedrich Wyrowski
Figure caption: Position−radial velocity diagram of the explosive streamers detected in IRAS12326−6245 with our ALMA observations. The PV diagram is made at the position of the center of the explosion (see text), and a PA of 77.°7. At this PA, we can elucidate three molecular streamers at high velocity. We have marked with white lines the streamers, and with a white circle the center of the explosion.
Paper: Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
Authors: Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati
Figure caption: Propagation of the GRB221009A across the heliosphere. The temporal profiles of the gamma-ray burst signal detected by the charged particle detectors on board STEREO-A, SolO, THC, Wind, and MAVEN are shown with different colors. T 0 = 13:16:59—time of the detection of the triggering impulse of GRB221009A in the vicinity of the Earth. y-axis—the distance between the points of observations along the normal to the signal front, where 0 is the position of the Earth. The normal was estimated based on the coordinates and times provided in the legend. Light-gray lines illustrate the propagation of Pulses 2, 3, and 4 of the GRB221009A with the speed of light.
Paper: Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
Authors: Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati
Figure caption: Detection of the effects of the GRB221009A by MAVEN: (a) electron flux by SWEA; (b) ion flux by SWIA; (c) electron counts by SEP; (d) ion rates by STATIC; (e)–(h) the integrated counts/rates from (a)–(d).
Paper: Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
Authors: Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati
Figure caption: Detection of the effects of the GRB221009A by the spacecraft of Earth group: (a) light curve by KONUS (Wind; data available at https://gcn.gsfc.nasa.gov/konus_grbs.html); (b) and (c) electron and ion flux by SST (Wind); (d) density of α-particles by PESA (Wind); (e) ions flux by ESA+SST (THC); (f) electron flux by MEPED (POES19); and (g) the integrated electron flux by MEPED (POES15, POES19, and MEtOp).
Paper: An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, Jan van Roestel
Figure caption: Hyades Gaia EDR3 color–magnitude diagram. Left: Current cluster members together with Parsec (Bressan et al. 2012) isochrones in purple (600–800 Myr, left to right) for a slightly metal-rich cluster (z = 0.024) with no reddening. Open circles are known variable or double stars (Perryman et al. 1998); these were not considered in deciding the age of the cluster, which we estimate at 675 ± 72 Myr. Carbon–oxygen WD cooling sequences (Bédard et al. 2020) shown in red are for 0.6–0.8 and 1.3 M ⊙ (right to left). Right: The same but for stars kinematically consistent with having escaped the Hyades cluster. The candidate ultramassive WD1 is plotted in green, and WD2 and WD3 are in blue.
Paper: SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise
Authors: T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Figure caption: Top: multicolor extinction-corrected light curves of SN 2022jli including photometric errors. Black lines along the bottom of the plot indicate spectroscopic observations. Open symbols are synthetic photometry performed on the EFOSC2 spectrum. Bottom: light curves after detrending with a second-degree polynomial fit including only the region after maximum light (vertical dashed line). Overplotted for each band are the best-fit sinusoids produced in the GLS analysis (Section 4.2). We retain the colors from the top panel and remove variation of point shape and do not include photometric errors for visual clarity, including only observations after MJD 59750.(The data used to create this figure are available.)
Paper: An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, Jan van Roestel
Figure caption: Candidate white dwarf escapees. Constant mass contours are shown from 0.2 to 1.3 M ⊙ (top right to bottom left), while age contours run horizontally for 50–800 Myr (top to bottom). Candidates selected for follow-up are labeled WD1–WD3 (green and blue). Orange points have total ages consistent with potential past cluster membership, but because their expected masses are below 1.0 M ⊙, they were not followed up. Black points are WDs that have kinematics consistent with having escaped the Hyades but appear to be too old for potential past cluster membership.
Paper: An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, Jan van Roestel
Figure caption: Left: Gemini-North GMOS spectrum for WD1, isolating the first four Balmer lines (black). The DA atmospheric model (Tremblay et al. 2011) fit is superimposed in solid red. Right: Photometric fit of WD1 using available Galex and Pan-STARRS photometry with 1σ error bars (blue). Black lines shows the synthetic spectrum computed from the best fit, with synthetic photometry shown in red.
Paper: SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise
Authors: T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Figure caption: Spectroscopic follow-up observation of SN 2022jli. Spectra are labeled by time since maximum light in the rest frame. Common SN lines are marked as vertical lines corresponding to the rest wavelengths. We include here the Grzegorzek (2022) classification spectrum. A TARDIS (Kerzendorf & Sim 2014) model of H- and He-free material is also included. Spectra for the Type Ic SNe SN 2004gk (Shivvers et al. 2019) and SN 1994I (Modjaz et al. 2014) were obtained from WISeREP (Yaron & Gal-Yam 2012).
Paper: An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, Jan van Roestel
Figure caption: Mass–radius relation at the approximate temperature of WD1 (26,000 K) for different compositions. The purple dashed curve is the expected core composition of WD1 formed from the expected mixture due to carbon burning including the effects of electron capture. Solid blue band shows the best fit and 1σ region for the radius obtained from photometry, while the orange and green bands show the same for the surface gravity and gravitational redshift determined from spectroscopy.
Paper: Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
Authors: Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati
Figure caption: Detection of the effects of the GRB221009A by SolO and STEREO-A: (a) light curves detected by STIX (SolO); (b) and (c) electron and ion flux from EPT (SolO); (d) electron counts from STE (STEREO-A); (e) and (f) integrated electron and ion counts from EPT (SolO); (g) integrated electron counts from STE (STEREO-A). The background light-gray silhouette is the light curves of the combined THC and THC SST proton flux counts from (Agapitov et al. 2023).
Paper: Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
Authors: Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati
Figure caption: The configuration of the spacecraft during the GRB211211A event: (a) location of STEREO-A, SolO, and MAVEN in the Heliocentric Inertial (HCI) coordinate system. The Earth’s orbit is shown in blue. (b) and (c) Locations of THEMIS and POES/MetOp spacecraft in the Geocentric Solar Ecliptic (GSE) coordinate system. The propagation of the GRB221009A across the heliosphere is schematically shown with the set of planes.