adsabs/AstroCLIMB huggingface dataset:
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Spectral energy distributions of the co-temporal X-ray, optical, and ultraviolet observations of GRB 180618A. The data after the white-band UVOT plateau (i.e., ≳ 200 s post-burst) are modeled with the following physical models. (a) Fast cooling of the electrons (χ 2/dof = 309/90). That is, we fix the optical spectral index to β opt = β opt,PI − 1 = 0.5, and we let the synchrotron frequency evolve as ν m ∝ t −1.5. (b) Slow cooling of the electrons (χ 2/dof = 330/90), i.e., we fix β X = β opt + 0.5 and the cooling frequency ν c ∝ t −0.5. (c) Fast cooling and a blackbody profile (χ 2/dof = 231/82). (d) Slow cooling and a blackbody profile (χ 2/dof = 106/82). The best-fitting optical spectral index is β opt  =  0.30 ± 0.08 (β X = β opt + 0.5), which corresponds to an electron index p = 1.6 ± 0.1. The dust contribution from the host galaxy is estimated to be E(B − V)HG < 0.02.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Artist impression of the different energy sources powering the GRB 180618A multiwavelength emission. (a) The material is equatorially ejected by tidal forces during the neutron star binary merger (Cucchiara et al. 2011) and radially ejected by hydrodynamic interactions at the neutron stars contact region (e.g., Metzger 2019). (b) The accretion of the torus onto a rotationally supported supramassive neutron star remnant (i.e., a millisecond magnetar) powers two relativistic jetted outflows (Bucciantini et al. 2012; Metzger et al. 2018) that, via internal dissipation mechanisms, produce the initial ≈0.3 s hard prompt gamma-ray emission. At this stage, the accretion disk releases winds that largely dominate the total mass ejected (Margalit & Metzger 2019). (c) The winds from the rotationally powered magnetar are collimated by the surrounding ejecta, which give rise to the ≈45 s duration soft gamma-ray emission (Bucciantini et al. 2012). (d) As the spin-down luminosity of the magnetar decreases, the jetted winds become stifled behind the ejecta, which is reheated at larger radii. When the opacity of the ejecta decreases sufficiently, bright optical thermal emission is emitted (Yu et al. 2013; Metzger & Piro 2014; Metzger 2019). (e) Hours after the merger, the ejecta is fully ionized by the winds of the long-lived magnetar, and the magnetar spin-down luminosity is detected (Metzger & Piro 2014).
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Spectral energy distributions of the co-temporal X-ray, optical, and ultraviolet observations of GRB 180618A. The XRT, UVOT, and RINGO3 data are modeled with the following synchrotron models. (a) Power laws (χ 2/dof = 292/159). (b) Broken power laws with a joint optical and X-ray spectral indexes (χ 2/dof = 170/158). The best-fitting spectral indexes are β opt  =  0.27 ± 0.02 and β X  =  0.84 ± 0.05. Note that we have fixed the break of the t 11 epoch (gray color) to the t 10 epoch value given the optical upper limits. In dotted lines, we show the best-fitting synchrotron model and in solid lines the model that includes the dust and hydrogen absorption from the Milky Way and host galaxy for a redshift z = 0.554. Detections have 1σ error bars, and nondetections are presented as 3σ upper limits.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Best-fitting models of the XRT X-ray light curve of GRB 180618A. (a) Broken power-law model. The best-fitting parameters are an initial decay rate of α X,1  =  0.79 ± 0.12, steeping to α X,2 = 1.77 ± 0.04 at t break = 162 ± 11 s (χ 2/dof = 131/102). (b) Broken power-law model plus a pulse function, with α X,1  =  0.99 ± 0.07, α X,2 = 1.89 ± 0.06, t break = 206 ± 14 s (χ 2/dof = 104/99). The bottom panels are the residuals of the best-fitting model.
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Intensity profiles vs. time taken at six different locations along the path of the comet. The dashed red line marks the time instant of the transit of the comet’s nucleus. The vertical dotted line indicates the moment at which the EUV emission starts to increase, hence when the oxygen ions start to emit. The time lag is calculated between these two vertical lines and must be corrected for the light travel time to the observer.
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Intensity profiles for the slits S4 and S5 as blue lines vs. squared density profiles obtained from the modeling (red line). For the density profiles, we applied a temporal shift (the values of t ⋆ in red) to better fit the rise of the intensity peak. The density profiles referred to the time of the comet’s transit (the values of t in black) are also shown as dashed gray lines. Different values of the parameters for these profiles as given inside square brackets. The vertical dotted black line represents the position of the beam front, computed from Equation (2) and analogous to the red points shown in the TD maps for slits S4 and S5.
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Time–distance maps relative to the slits S1–S6 marked in Figures 4 and 5. The position of the beam as a function of time obtained from Equation (2) at time steps of 24 s are overplotted as red dots in the TD maps for slits S4 and S5. For details, see Section 4.2.
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Intensity profiles for the slits S1–S3 and S6 recorded with SDO/AIA (blue lines) and compared with the squared density profiles obtained from the modeling (red lines).
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Left panels: composite images taken at different times with SDO/AIA in the 171 channel and showing the tail of striae left by Comet Lovejoy enclosed within two continuous red lines before (top panels) and after (bottom) the transit at the perihelion. The orbit of the comet is shown as a dotted red line. Right panels: blow-up view of the regions where striae are formed. The corresponding regions are outlined with a dashed red box in the left panels. The filled green circles labeled by letters mark the locations where intensity profiles are extracted and plotted in Figure 2.
Paper: Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy
Authors: Giuseppe Nisticò, Gaetano Zimbardo, Silvia Perri, Valery M. Nakariakov, Timothy J. Duckenfield, Miloslav Druckmüller
Figure caption: Scheme of the mechanism for the formation of the striae.
Paper: Coronal Mass Ejection Deformation at 0.1 au Observed by WISPR
Authors: Carlos R. Braga, Angelos Vourlidas, Paulett C. Liewer, Phillip Hess, Guillermo Stenborg, Pete Riley
Figure caption: The CME observations on 2021 January 21 around 03:30 (middle row), its GCS modeling projected over each observation (top row), and its synthetic images (bottom row).
Paper: High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy 
Authors: Jennifer E. Andrews, Jeniveve Pearson, M. J. Lundquist, David J. Sand, Jacob E. Jencson, K. Azalee Bostroem, Griffin Hosseinzadeh, S. Valenti, Nathan Smith, R. C. Amaro, Yize Dong, 宜泽 董, Daryl Janzen, Nicolás Meza, Samuel Wyatt, Jamison Burke, Daichi Hiramatsu, D. Andrew Howell, Curtis McCully, Craig Pellegrino
Figure caption: Spectral comparison between SN 2019esa (316 days post maximum) and SN 2006gy (287 days post maximum) in luminosity space. SN 2006gy spectra are from Kawabata et al. (2009). Both spectra have been dereddened and we have used the distance and reddening adopted for SN 2006gy from Jerkstrand et al. (2020). The line strengths are almost identical in both spectra except for the stronger Ca emission in SN 2019esa.
Paper: Coronal Mass Ejection Deformation at 0.1 au Observed by WISPR
Authors: Carlos R. Braga, Angelos Vourlidas, Paulett C. Liewer, Phillip Hess, Guillermo Stenborg, Pete Riley
Figure caption: The CME observations on 2021 January 20 around 23:30 (middle row), its GCS modeling projected over each observation (top row), and its synthetic images (bottom row).
Paper: Coronal Mass Ejection Deformation at 0.1 au Observed by WISPR
Authors: Carlos R. Braga, Angelos Vourlidas, Paulett C. Liewer, Phillip Hess, Guillermo Stenborg, Pete Riley
Figure caption: Position of the three observing spacecraft (circles). As PSP position changes significantly while WISPR observes the CME observation (from 2021 January 20 21:00 UT to 2021 January 22 17:00 UT), we indicate the spacecraft position at the first and last observations here (red and magenta circles). The lines with origins at each PSP position indicate WISPR-I and WISPR-O FOV limits.
Paper: Coronal Mass Ejection Deformation at 0.1 au Observed by WISPR
Authors: Carlos R. Braga, Angelos Vourlidas, Paulett C. Liewer, Phillip Hess, Guillermo Stenborg, Pete Riley
Figure caption: Multiple observations from STEREO-A indicating the solar origins of the CME: (a) EUVI 304 showing the prominence; (b) EUVI 195; and (c) EUVI and COR1 combined.
Paper: High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy 
Authors: Jennifer E. Andrews, Jeniveve Pearson, M. J. Lundquist, David J. Sand, Jacob E. Jencson, K. Azalee Bostroem, Griffin Hosseinzadeh, S. Valenti, Nathan Smith, R. C. Amaro, Yize Dong, 宜泽 董, Daryl Janzen, Nicolás Meza, Samuel Wyatt, Jamison Burke, Daichi Hiramatsu, D. Andrew Howell, Curtis McCully, Craig Pellegrino
Figure caption: Spectral comparison between SN 2019esa and SN 2006gy before maximum (top) and near maximum (bottom). SN 2006gy spectra are from Smith et al. (2007). All spectra have been corrected for reddening and all epochs are with respect to the date of r/R-band maximum.
Paper: Variable Star Classification with a Multiple-input Neural Network
Authors: T. Szklenár, A. Bódi, D. Tarczay-Nehéz, K. Vida, Gy. Mező, R. Szabó
Figure caption: Gallery of lightcurve images of the different variable star types used in this work. The light curves are from the OGLE-III catalog; pulsating variable stars and eclipsing binaries are phase folded in the [0..2] interval by their pulsating periods and the orbital periods, respectively. Images, from top to bottom, in each row represent ACep, Cep, DSct, ECL, RRLyr, and T2Cep variable stars. This gallery only shows light curves with real measurements and they were resized and have 128 × 128 pixel resolution as was used in the first input of the neural network.
Paper: Variable Star Classification with a Multiple-input Neural Network
Authors: T. Szklenár, A. Bódi, D. Tarczay-Nehéz, K. Vida, Gy. Mező, R. Szabó
Figure caption: Gallery of artificially generated phase-folded lightcurve images. The first column shows the original light curves, of which the synthetic data were generated. The rows correspond to the following variable star subtypes: ACep 1O, ACep F, DSct Multimode, T2Cep BLHer, T2Cep, RVTau, and T2Cep WVir. Most of the artificial light curves were generated for these subtypes. The lightcurve images shown in this figure were resized and have 128 × 128 pixel resolution as they were used in the neural network.
Paper: Variable Star Classification with a Multiple-input Neural Network
Authors: T. Szklenár, A. Bódi, D. Tarczay-Nehéz, K. Vida, Gy. Mező, R. Szabó
Figure caption: Gallery of some variable star subtypes to show the process of synthetic data generation using Gaussian process (GP) regression. Top: black points are the original phase-folded light curves with their uncertainties (gray bars). The red lines are the mean of GP predictions, and the shaded orange areas show the three standard deviations from the mean. Bottom: the artificially generated phase-folded light curves that were randomly sampled from the GP posteriors at random phase values.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The PV diagrams of 12CO (gray scale) and 13CO (green contours) along the filaments. The green contours are set from 3σ to the peak value in steps of 3σ. The color bar is in units of kelvins. In order to preserve the velocity continuity, pixels above 2σ are kept to construct the 13CO m1 profiles (cyan dotted lines). The blue lines are the linear fitting results of the corresponding segments. The corresponding velocity gradients in units of km s−1 pc−1 and the mass flow rates in units of M ☉ Myr−1 are marked beside. The symbols of black squares, red solid circles, and magenta crosses are the star formation sets of H II regions, IRAS sources, and intersection points between filaments. The red and green intervals mark out the highlighted areas in Figure 18.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The distribution of the candidate YSOs. The gray-scale background is the H2 column density map estimated from 12CO. The black dashed lines are the filament skeletons identified in Figure 6. The gray contours represent the 3σ boundary of the 12CO emission (0.2 × 1021 cm−2). The magenta, green, and blue crosses represent the candidate YSOs of Class I, the flat type, and Class II, respectively. The red circles with plusses indicate the candidate YSOs with luminosities greater than 100 L ⊙.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The normalized second-order SFs of velocity (blue solid lines) and column density (red solid lines). In order to keep the velocity consistent, the intensity-weighted mean velocity of 12CO along each filament is used to construct the velocity profiles. The column density estimated from 13CO is used to construct the density profile. Pixels above 3σ are kept in the process. The blue and red shaded areas indicate the standard deviation ranges of the SF profiles. The vertical blue and red dashed lines indicate the potential characteristic length scales of periodic fluctuations in velocity and density. The dark gray shaded area indicates the range of lags below the spatial resolution of the data.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The velocity field maps (moment 1) of 12CO (upper panel) and 13CO (bottom panel). The black arrow lines indicate the extended paths according to the 12CO emission. The name of each filament is marked beside it. The symbols of squares, solid circles, and magenta crosses represent the associated H II regions, the IRAS sources, and the intersection positions between filaments, respectively. The coordinates (l, b) of the intersections are for cross A ∼﹩\left(154\buildrel{\circ}\over{.} 531,2\buildrel{\circ}\over{.} 479\right)﹩, for cross B ∼﹩\left(154\buildrel{\circ}\over{.} 452,2\buildrel{\circ}\over{.} 754\right)﹩, and for cross C ∼﹩\left(154\buildrel{\circ}\over{.} 556,2\buildrel{\circ}\over{.} 638\right)﹩.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The mass vs. radius diagram of the 13CO clumps. The green line and red line represent the lower limits of high-mass star formation (﹩{M}_{c}=870\,{M}_{\odot }{\left(R/\mathrm{pc}\right)}^{1.33}﹩) from Kauffmann et al. (2010) and 0.05 g cm−2 from Urquhart et al. (2013). The linear-fitted slope and correlation coefficient of the clump sample are labeled in the upper right corner.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: A composite three-color image of three WISE bands (22 μm in red, 4.6 μm in green, and 3.4 μm in blue). The white contour represents the 3σ boundary of the 13CO emission. The red circles are the locations of the three H II regions. The nine green circles indicate the regions where mass flow activity is detected.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: Luminosity function of the YSO sample (left panel) and the sources that are located within the cloud (right panel). The red vertical line is the position of 100 L ⊙.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: Histograms of the 3D velocity dispersion (left panel), and 1D thermal (middle panel) and nonthermal (right panel) velocity dispersions of the 13CO clumps. The ranges and median values are marked on each panel.
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: The 13CO velocity-integrated intensity map (moment 0) overlapped with the clumps color-scaled by α vir. The black dashed lines are the same as those in Figure 6.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: The sensitivities of DR to Ω m  and w, quantified by ∂lnDR/∂Ω m  (left panel) and ∂lnDR/∂w (right panel). The results for H(z) are plotted for comparison. For identical fractional measurement error, the constraint of Ω m  from DR will be a factor of 4 better than that from H on the median, and constraint of w from DR will be a factor of 7 better than that from H for 0 < z < 1. A cosmology of Ω m  = 0.3 and w = −1 is used for the plots.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: The lensing potential-LDP cross correlation measured with different filters upon the masked CMB lensing potential. Green dashed line: without applying any filter to the lensing potential. Red solid line: applying a top hat filter of 5 <ℓ < 1024 to the lensing potential Φ ℓ m . Purple dotted line: applying a top hat filter of 0 < ℓ ≤ 5. Blue dashed–dotted line: applying a top hat filter of 20 < ℓ < 1024.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: Constraints on the flat wCDM model, from BAO/DR/BAO+DR (left panel) and SN/DR/SN+DR (right panel). Partly due to the Ω m –w degeneracy direction and partly due to its higher sensitivity on Ω m  and w, the inclusion of DR significantly improves over BAO or SNe alone.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: Improvement in wCMD constraints by including the DR measurement. “Peak” refers to the best-fit value of the parameter and “mean” refers to the average value of the parameter. The improvement in parameter uncertainty is 1.4–2. ﹩\left|\mathrm{decl}.\gt 30^\circ \right|﹩ is an additional mask adopted to all maps used for deriving the main results in this paper (solid lines). We also show the results obtained without adopting this mask for comparison (dotted lines), which are consistent with the solid lines.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: The probability distribution function of DR (blue solid line) obtained by the estimator of Equation (A1). It is well described by a Gaussian function (blue dashed line), for which we list the best-fitting values of the PDF. The PDF is normalized with its peak amplitude.
Paper: The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint
Authors: Fuyu Dong, Pengjie Zhang, Zeyang Sun, Changbom Park
Figure caption: The gravitational potential decay rate (DR) measured at 0.2 < z < 0.4, 0.4 < z < 0.6 and 0.6 < z < 0.8. Red (green) data points show the results obtained with LDPs (galaxies). Theoretical curves of five wCDM cosmologies are also shown for demonstration.