adsabs/AstroCLIMB huggingface dataset:
Paper: Atomic Data for Astrophysically Important Spectral Lines of Singly Ionized Nitrogen
Authors: M. C. Li, W. Li
Figure caption: Comparison of the present ﹩\mathrm{log}({gf})﹩ values in the Babushkin gauge with the corresponding values adopted by M. F. Nieva & N. Przybilla (2012) for abundance analysis and also with the available values from CIV3 calculations by K. L. Bell et al. (1995).
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: Example gas temperature map (upper panels) and shock-dissipated energy map (lower panels) of MGS systems with prominent bow shocks. These MGS halos with M 200 > 1014 M ⊙ have neighboring MGS halos with M 200 > 1013 M ⊙ within a 3 Mpc boundary. The gas temperature map of 12 other candidates with bow shock is in the Appendix.
Paper: Atomic Data for Astrophysically Important Spectral Lines of Singly Ionized Nitrogen
Authors: M. C. Li, W. Li
Figure caption: Percentage fractions of all transitions in different uncertainty categories for the uncertainties estimated based on d T values only (orange), d T&CF (green), ﹩d\widetilde{T}﹩ (purple), and ﹩{\rm{d}}\widetilde{T}﹩&CF values (yellow).
Paper: Atomic Data for Astrophysically Important Spectral Lines of Singly Ionized Nitrogen
Authors: M. C. Li, W. Li
Figure caption: Comparison of present transition rates, A, in Babushkin gauge, with the corresponding experimental results published by S. Mar et al. (2000) and J. Musielok et al. (1996).
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: Same as Figure 8, but for the rest of the merging cluster candidates with bow shocks.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: Same as Figure 10, but for t = 0.3 to 0.6 Myr, respectively.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Light curves of the TDEs that did not show clear variability over the span of the RACS observations (roughly 3 yr) and might be contaminated by host emission: AT 2022dsb (purple), AT 2022bdw (orange), AT 2021qxv (red), AT 2020zso (cyan), ASASSN-20mi (brown), and ASASSN-14li (magenta). For each TDE the RACS-low data are shown as stars, RACS-mid data as squares, RACS-high data as circles, and the VLASS data as diamonds. Filled markers represent detections and open markers represent upper limits. The black dashed line shows the optical outburst time. Where possible, we use RACS+VLASS measurements to estimate the slope of the power-law spectrum (see Section 3.6).
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: WISE color–color plot showing the magnitude difference in band 1 (W1) and band 2 (W2) on the y-axis, and band 2 (W2) and band 3 (W3) on the x-axis. The contours for different object classes are adopted from Wright et al. (2010). We used a W1 − W2 color of >0.8 to classify an object as an AGN.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Blackbody luminosity vs. temperature of the nonrelativistic TDEs detected by various surveys. The background gray circles show the optical sample from the ZTF (Hammerstein et al. 2023; Yao et al. 2023) that are within a redshift of z = 0.1 and the blue circles show the TDE sample with z > 0.1. The red stars show the optically discovered TDEs that are detected in our radio sample. The purple squares show the optically discovered TDEs that resulted in radio detections in a targeted follow-up study by Cendes et al. (2024). The green diamonds show the TDEs that are independently identified in radio by Somalwar et al. (2023), but then confirmed optically. Where multiple points overlap, sources are common to multiple samples.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Top panel: light curve of the TDE AT 2019qiz using RACS, VLASS, and archival data at four different frequencies from 5.5 to 21 GHz from O’Brien et al. (2019a, 2019b). The green stripe shows the multifrequency epoch at ∼75 days, which we use for spectral fitting. The black dotted line shows the 3σ predisruption limit from VLASS data and the red dotted line shows the same from RACS-low epoch 1 data. Bottom panel: spectrum of this transient using observations at four different frequencies taken at the same epoch (∼75 days post optical discovery; indicated by the box in the top panel). The orange line is the best-fit broken power law to the observed spectrum (see Section 3.5). The dashed black line is the best-fit single power-law spectrum (with spectral index α = 0.64).
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Estimates of equipartition radius and minimum total energy of the system, where possible, for the TDEs in our sample and archival TDEs (taken from Cendes et al. 2024). For our sample of TDEs, estimates derived from this study are shown as stars and those from the archival studies (Horesh et al. 2021; Cendes et al. 2022; Christy et al. 2024) are shown as colored circles. Estimates for archival TDEs that show late-time activity are shown as black dots (adapted from Cendes et al. 2024).
Paper: Recurrent Coronal Mass Ejections and Their Geomagnetic Storms Association on 2012 January 19: Solar Surface to Upper Earth’s Atmosphere Analyses
Authors: A. Hassanin, Amira Shimeis, Hadeer F. Sabeha, F. N. Minta
Figure caption: Contemporaneous difference images captured by SDO/AIA full-disk images and SOHO/LASCO-C2 with FOV from 2 R ⊙ to 6 R ⊙, showing CME1, CME2, and CME3, each accompanied by their respective source locations.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: The radio luminosity of the five strong TDE detections in the RACS data set at 887.5 MHz. The solid line shows radio luminosity from RACS detections while the dashed lines show the same from 5–7 GHz (data adapted from Horesh et al. 2021; Cendes et al. 2022; Goodwin et al. 2022b; Christy et al. 2024). Shown in gray in the background are the light curves (at 6 GHz) of the archival TDEs detected by Cendes et al. (2024) and Alexander et al. (2020) from optically selected TDEs.
Paper: Radio Afterglows from Tidal Disruption Events: An Unbiased Sample from ASKAP RACS
Authors: Akash Anumarlapudi, Dougal Dobie, David L. Kaplan, Tara Murphy, Assaf Horesh, Emil Lenc, Laura Driessen, Stefan W. Duchesne, Hannah Dykaar, B. M. Gaensler, Timothy J. Galvin, Joe Grundy, George Heald, Aidan W. Hotan, Minh Huynh, James K. Leung, David McConnell, Vanessa A. Moss, Joshua Pritchard, Wasim Raja, Kovi Rose, Gregory Sivakoff, Yuanming Wang, Ziteng Wang, Mark H. Wieringa, Matthew T. Whiting
Figure caption: Light curve of TDE AT 2020nov using RACS, VAST, and VLASS data, all resulting in detections, with very little variability. The green stripe shows the data points used to measure the spectral index of the power-law spectrum.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Spectral evolution of SN 2022crv in the 1 and 2 μm regions. The phase is measured from the dates of explosion and V-band maximum light. Feature A can be fit with a two-Gaussian function. The velocity scales of C I λ1.0693 μm, Mg I λ1.0927 μm, high-velocity He I λ1.083 μm, Fe II λ1.05 μm, S I λ1.0457 μm, and Sr II λ1.0327 μm are shown in the top abscissa axis. In the left panel, the red dashed line roughly marks the position of feature A at 1.005 μm, corresponding to ∼23,280 km s−1, assuming feature A is from He I λ1.083 μm. The red dashed line in the right panel also has a velocity of ∼23,280 km s−1 with respect to He I λ20,581. The gray dashed line marks the possible identification of Sr II λ1.0036 μm, at a velocity of ∼8000 km s−1.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: NIR spectra of SN 2022crv. The phase is measured from the dates of explosion and V-band maximum brightness. The red dashed line marks the extra absorption feature on the blue side of He I λ1.083 μm. The high telluric absorption regions are marked with gray bands. These spectra are available in machine readable format at the 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: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Late-time profile of [O I] λ λ 6300, 6364 and [Ca II] λ λ 7291, 7323. The phase is measured from the explosion. The zero-points for [O I] and [Ca II] are 6300 Å and 7307.5 Å, respectively, and are marked by the solid vertical lines in each panel. The black vertical dashed line in the left panel indicates 6364 Å. The blue vertical dashed line corresponds to the blueshifted peak around 6270 Å.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Comparison of the optical spectra of SN 2022crv 2.7 and 17.7 days after the explosion with models from L. Dessart et al. (2016) and S. E. Woosley et al. (2021) at similar epochs. The 6200 Å feature is marked by the blue shading. The He3.40 and He5.38 models are hydrogen-free models, while the 3p65Ax2 and 3p0Ax1 models retain a small amount of hydrogen.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: An SVM time-dependent spectral classification of SN 2022crv (M. Williamson & M. Modjaz 2024, in preparation) based on the methods presented by M. Williamson et al. (2019). SN 2022crv is classified as an IIb SN IIb before around −10 days from the V-band maximum brightness. After that, SN 2022crv is more similar to an SN Ib. The trajectory in principal component analysis phase space as SN 2022crv evolves (magenta) clearly shows the type of transition occurring in the spectra.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Upper: the pEW evolution of the 6200 Å feature of SN 2022crv compared with other SESNe. The 6200 Å feature in SN 2022crv shows a large pEW at the beginning, similar to other SNe IIb. Then, it quickly decreases until it disappears around 15 days after ﹩{V}_{\max }﹩. Bottom: velocity evolution of the 6200 Å feature in SN 2022crv, assuming it is from Hα. The velocity of the 6200 Å feature in SN 2022crv is generally larger than that in SNe IIb but similar to that in SNe Ib.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Line identification of the nebular spectrum taken on day 272.3 (290.6 days after the explosion). A double Gaussian function is fitted around each of 6300 Å and 7300 Å, to respectively deblend [O I] and [Ca II] from other lines. The continuum is defined by a straight segment connecting the two local minima.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Observed spectra of SN 2022crv compared with the mean spectra (the solid lines) and the standard deviations (the shaded regions) of SNe IIb, Ib, and Ic from Y.-Q. Liu et al. (2016). The observed spectra have been flattened using SNID.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Comparison of combined optical and NIR spectra of SN 2022crv with those of other SNe Ib/IIb. The positions of Hα (black dashed line) and 1.005 μm (red dashed line) are marked.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Best-fit SED of GBM data using a combination of the Band function and BB model. The purple dotted–dashed line and green dotted–dashed represent the Band component and BB component, respectively. Solid dashed lines represent the ν F  ν  spectra resulting from the combination of these two models, and the red shade shows the 1σ error.