adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: TRAPPIST-1 e NIRSpec/PRISM transmission spectra on different epochs for different pipelines. Analogous to Figure 2 but comparing the transmission spectra obtained by different pipelines/reductions in our team. Note that reductions with the same pipelines by different individuals are plotted with similar colors (i.e., transitspectroscopy reductions by NE and AG are in blue, Eureka! reductions by SC/KS and CC are in orange/red, ExoTiC reductions are in green). This is done on purpose for ease of comparison between varying parameters within a given pipeline and comparing reductions with truly different pipelines. Note that we compare the median-subtracted transmission spectrum across different pipelines, as our inference described in Section 3 does not depend on the absolute transit depth level but on the shape of the transmission spectra.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Representative example of implantation of a planetesimal that arrives relatively early in the belt, at about ∼40 Myr. The early arrival of this object in the asteroid belt makes it most likely inconsistent with Athor. As in Figure 1, the x-axes show time, and the y-axes show, from top to bottom, semimajor axis, orbital eccentricity, and inclination. Dashed lines delimit the Athor region, defined as 2.3 au < a < 2.5 au, e < 0.15, and i < 15°. This simulation corresponds to an example where the instability also takes place at the time of the disk dispersal, tinst = 5 Myr, relative to the solar system formation time. The final implantation of this planetesimal happens at about 85 Myr, when Krios is ejected from the system.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: TRAPPIST-1 e NIRSpec/PRISM transmission spectra on different epochs. The transmission spectra are ordered in chronological order from top to bottom, with the dates on which they were obtained indicated in the lower right of each panel. The y-axes for all plots cover the same ranges, which highlight how much the transmission spectrum varies across epochs—in particular for the transmission spectra obtained in 2023 July and October.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: TRAPPIST-1 e stellar contamination retrievals. Retrievals are carried out with exoretrievals on the NE reduction. All models shown use the BT-SETTL stellar models. Left panel: the first and second visits and the best-fit cold-spot model, which is approximately consistent between visits. Middle panel: the third visit, along with hot-spot models from both the mask 1 and mask 2 retrieval tests as described in the text. Here it can be seen that (a) stellar contamination predicted in the longer wavelengths from that seen in the shorter wavelengths does a poor job at matching the observations, and (b) stellar contamination models do a poor job of matching the 1–3 and 3–5 μm regions simultaneously. Right panel: the fourth visit with the best-fit hot-spot model. Similar to point (b) from the middle panel, the stellar contamination model cannot fit both the middle wavelengths and the longer wavelengths well.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: The TRAPPIST-1 e HST/WFC3 transmission spectra presented in Z. Zhang et al. (2018) interpreted with GPs and an atmospheric model. (Left) Transmission spectra of the two HST/WFC3 visits (black points with error bars) modeled with a GP times an atmospheric model (gray), analogous to the top panels in Figure 3. Bands represent 1σ and 3σ credibility. (Right) Visit-combined transmission spectrum obtained by averaging the two WFC3 visits after correcting for the modeled GP component (black points with error bars). The atmospheric model is in gray. Bands represent 1σ and 3σ credibility. This is analogous to the bottom panel of Figure 3. Note that we use the very same y-limits in this figure and in Figure 3.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: Atmospheric and GP hyperparameter posterior distributions. Posterior distribution of some of our JWST NIRSpec/PRISM retrieval parameters, compared to the atmospheric parameters we constrain in this work in Figure 4, H2 and cloud-top pressure/surface pressure. Note how the GP hyperparameters (length scales ℓi and amplitudes Ai) do not show strong correlations with the atmospheric parameters.
Paper: Discovery of the Second Y+Y Dwarf Binary System: CWISEP J193518.59-154620.3
Authors: Matthew De Furio, Jacqueline Kelly Faherty, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Eileen C. Gonzales, Rocio Kiman, Marc Kuchner, Federico Marocco, Sherelyn Alejandro Merchan, Melanie Rowland, Adam C. Schneider, Genaro Suárez, Johanna M. Vos
Figure caption: F1000W vs. F1000W–F1280W color–magnitude diagram for all sources observed with MIRI in GO–2124, overplotted with the ATMO2020 isochrone for 5 Gyr (M. W. Phillips et al. 2020) and Sonora Bobcat isochrone for logg = 4.0 and solar metallicity (M. S. Marley et al. 2021) with select effective temperatures shown in red. All photometry for sources without known companions is shown in black, the combined photometry for W1711, W0146, and W1935 is shown in magenta, the photometry for the primary of each of the three binary systems is shown in red, and the photometry for the companions is in blue. Photometry was taken from J. K. Faherty et al. (2025, in preparation). Absolute magnitudes were computed assuming distances from J. D. Kirkpatrick et al. (2021). From only the photometry, W1935B would be the faintest and coldest object observed in this sample, with an estimated effective temperature of ∼350–375 K assuming the Sonora Bobcat models. Nearly all sources seem bluer than the models, which may impact their estimated effective temperature and mass.
Paper: Discovery of the Second Y+Y Dwarf Binary System: CWISEP J193518.59-154620.3
Authors: Matthew De Furio, Jacqueline Kelly Faherty, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Eileen C. Gonzales, Rocio Kiman, Marc Kuchner, Federico Marocco, Sherelyn Alejandro Merchan, Melanie Rowland, Adam C. Schneider, Genaro Suárez, Johanna M. Vos
Figure caption: As in Figures 1 and 2, we simultaneously fit for the companion to W0146 and W1711 across all filters and dither positions. We show an example of one dither position for W0146 in F1000W with the single-PSF fit in the top row and double-PSF fit in the second row. As expected, the residuals follow the pattern for a good model fit to the data, i.e., random noise, for the double fit and structured residuals for the single fit. In the bottom row, we show an example of one dither position for W1711 in F1000W from the double-PSF fit, which is also resolvable by eye.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Left: bolometric light curve of SN 2024uwq, along with the evolution of temperature (black) and photospheric radius (green). The bolometric light curve and blackbody temperatures TBB of SN 2024uwq are compared with those of other SNe IIb in the literature when available. In the bottom TBB− RBB panel, the overplotted comparison points represent TBB only. Shock cooling models are valid only for data where the TBB is greater than 8120 K or 0.7 eV (see N. Sapir & E. Waxman 2017) Right: bolometric light-curve fit with a two-component Arnett model using MCMC. Black and gray lines depict two- and one-component models, respectively (150 random draws from the posterior); orange and green trace inner and outer ejecta contributions, respectively. Observational data are shown in blue with 1σ uncertainities.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Progenitor radius vs. envelope mass for SNe IIb, including SN 2024uwq. All best-fit values of all four models are shown, with each filling style of the marker indicating the respective model. For the SNe highlighted in bold, where the comparison values are from shock cooling modeling, we plot the available respective model values in the literature. Published values for other SNe in this figure are obtained from S. E. Woosley et al. (1994; SN 1993J), A. Pastorello et al. (2008) and R. A. Chevalier & A. M. Soderberg (2010; SN 2008ax), M. C. Bersten et al. (2012; SN 2011dh), D. Milisavljevic et al. (2013; SN 2011ei), A. Morales-Garoffolo et al. (2015; SN 2011fu), A. Morales-Garoffolo et al. (2014; SN 2013df), I. Arcavi et al. (2017; SN 2016gkb), P. Armstrong et al. (2021; SN 2017jgh), C. Pellegrino et al. (2023; SN 2020bio), J. R. Farah et al. (2025; SN 2022hnt), and A. Reguitti et al. (2025) and K. K. Das et al. (2023; SN 2024abfo).
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Top: NIR spectra of SN 2024uwq at +76 days obtained using Gemini F-2. The gray bands mark the regions with high telluric absorptions and emissions. Bottom: The CO first-overtone feature of SN 2024uwq (in red) shows strong resemblance to those observed in the SN IIb SN 2011dh and is also compared with those of the SN IIP SN 2017eaw. The vertical dashed lines mark the band heads of Δv = 2 transitions.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Optical spectra of SN 2024uwq showing temporal evolution from +4 to +64 days, with respect to our assumed explosion epoch of MJD 60558.63. The most prominent lines in the spectra are identified. Spectroscopic data used in this figure are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Early-time light curve of SN 2024uwq with shock cooling model fits. Each panel represents the individual shock cooling model. The family of model light curves in each panel represents 50 models randomly sampled from the derived posterior probability distribution in individual bands. The best-fit values and prior distributions of the physical parameters for each model considered in this work are listed in Table 2.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Top: multiepoch spectral evolution of Hα (λ6563) and He I (λ5876), observed between +4 and +64 days. The Hα emission-line profile evolution is strongly affected by He I λ6678 line emergence. Bottom: velocity evolution of SN 2024uwq derived from P Cygni minima of Hα and He I, shown relative to explosion epoch and in comparison to other SNe IIb.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Simulated ULTRASAT NUV and Swift UVW1 light curves, demonstrating ULTRASAT’s detectability of complete SCE phases out to 200 Mpc. Photometry was simulated using the SED of SN 2024uwq at each epoch convolved with the respective filter throughput. The error bars represent the photometric uncertainties.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Comparison of the optical spectra of SN 2024uwq at +4 days (top), +20 days (middle), and +46 days (bottom) with other SNe IIb. The spectra have been redshift corrected and shifted vertically for clarity.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Evolution of the blackbody temperature (TBB) as a function of phase from explosion for UV + optical and optical-only observations. The inclusion of UV data provides better constraints on the SED peak, resulting in more accurate temperature estimates and reduced uncertainties, particularly at early times.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: Moth plots, 2D histogram, of temperature ratio (TO6+/Tp) for differential streaming of O6+ normalized to the local Alfvén speed vs. angle (Θ) between the radial direction and the local magnetic field direction. The color bar indicates the proton-to-O6+ temperature ratio (TO6+/Tp), which is kept consistent across all panels and with Figure 1.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: The magnetic field and velocity, radial (BR, VR), and perpendicular projections (B⊥, V⊥) during the shaded magenta region time frame of Figure 4, where the color of the points indicates the associated time.
Paper: Observational Constraints on the Radial Evolution of O6+ Temperature and Differential Flow in the Inner Heliosphere
Authors: Yeimy J. Rivera, Kristopher G. Klein, Joseph H. Wang, Lorenzo Matteini, Daniel Verscharen, Jesse T. Coburn, Samuel T. Badman, Susan T. Lepri, Ryan M. Dewey, Jim M. Raines, B. L. Alterman, Timothy J. Stubbs, Kevin C. Delano, Roberto Livi, Stefano A. Livi, Antoinette B. Galvin, Christopher J. Owen, Michael L. Stevens
Figure caption: (Left) 2D histogram of counts of differential speed, VO6+,p, against Alfvén speed, VA. The green line has a slope of 1 showing correlation between the values. (Right) Radial evolution of Alfvén speed within the same speed bins as Figure 2. We include three power-law profiles, 1/r0.7, 1/r0.8, and 1/r1, for reference.
Paper: Detection of Low-redshift Excess in Supernova-linked Gamma-Ray Bursts
Authors: Qin-Mei Li, Qi-Bin Sun, Sheng-Bang Qian, Fu-Xing Li
Figure caption: Left: the distribution of cumulative luminosity function ψ(L0), which is normalized to unity at the lowest luminosity. The function is fitted by a red solid line with a broken power law. The luminosity function can be expressed as ﹩\psi ({L}_{0})={L}_{0}^{-0.14\pm 0.01},{L}_{0}\lt {L}_{0}^{b}﹩ and ﹩\psi ({L}_{0})={L}_{0}^{-0.70\pm 0.03},{L}_{0}\gt {L}_{0}^{b}﹩. Right: normalized cumulative redshift distribution.
Paper: Detection of Low-redshift Excess in Supernova-linked Gamma-Ray Bursts
Authors: Qin-Mei Li, Qi-Bin Sun, Sheng-Bang Qian, Fu-Xing Li
Figure caption: Comparison SN/GRBs rate and SFR. The SFR data and fit line were collected from P. Madau & M. Dickinson (2014; brown dots). The blue line is the formation rate of fitting 56 SN/GRB sources. The error bar gives a 1σ Poisson error.