adsabs/AstroCLIMB huggingface dataset:
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:                         The N(H2) maps for t = 0.1 to 0.7 Myr in the x–z (at left), y–z (middle), and x–y (right) planes, respectively. The plus (+) symbols represent the positions of the sink particles. The white plus symbol shows the heaviest sink particle. The positions of two massive sink particles at t = 0.7 are marked in white and cyan, with two arrows pointing toward them in panel (u). The gray dashed circular regions overlaid on the N(H2) maps in the x–y plane from t = 0.2 to 0.7 Myr are zoomed-in in Figure 8 with identical color scales. Identical circular regions and color scales from t = 0.3 to 0.7 Myr are presented in Figure 9. The pair of horizontal and vertical white lines highlighted on panel (i) are utilized to extract the PV diagrams, which are shown in Figure 11.
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: Panels (a)–(h) present histograms of H2 density for each pixel within the range of z: [−2, 2] pc, for t = 0.0 to 0.7 Myr, respectively. Each panel also includes the maximum and minimum density values (i.e., ﹩{n}_{\max }﹩ and ﹩{n}_{\min }﹩, respectively) at the corresponding time. The blue dotted line on the panels (b)–(h) is at n = 102 cm−3.
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: Panels (a)–(f) display the N(H2) map in the y–z plane for the range of x: [−1, 1] pc. In each panel, the overlaid cone illustrates the conical structure of the shock-compressed layer, and a blue arrow indicates its angle with respect to the z-axis. The angle is also mentioned in each panel.
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: An illustration of the initial setup for CCC, similar to T. Inoue et al. (2018): (a) The H2 column density (i.e., N(H2)) map in the y–z plane. The arrows in color light-coral point out the directions of movement for the cloud components. The black arrow indicates the direction of the magnetic field. Panels (b) and (c) present the density and z-component of the velocity distribution of the molecular gas along the z-axis, respectively. The spherical cloud component and the sea of dense gas are specified in each panel. In panel (b), the directions of movement of the cloud components are shown with two arrows. In panel (c), the extent of the spherical cloud component is marked with gray dotted lines.
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: Panels (a)–(f) depict the distribution of dense molecular gas along the z-direction for t = 0.2 to 0.7 Myr for the cone-shaped compressed layers shown in Figure 4. However, the z-axis range is extended and made identical for each time. The thinnest, intermediate, and thickest lines represent density thresholds of n > 104, n > 105, and n > 106 cm−3, respectively.
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: The mass-weighted average (a) density and (b) z-component of velocity, and (c) gravitational acceleration of the cone-shaped compressed layers for t = 0.2 to 0.7 Myr as highlighted in Figure 4.
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: Shows the signatures of ICME/IP shock observed from 2012, 21 to 27. The ICME plasma field was evident between January 22 06:12 UT and January 24 00:00 UT. (A)–(I) panels show the total IMF (nT), Bx, By, Bz components of magnetic field strength (nT), Solar wind speed (km s−1), proton density (np/cc), proton temperature (K), flow pressure (nPa), Al index, plasma Beta, and high-resolution SYM-H (nT), respectively. The shaded portion in sky blue represents the period between the arrival of the ICME/shock at the vicinity of the Earth and its cessation. This region also describes the ICME as a magnetic cloud (MC) with a turbulent sheath defined by the spacing between the boundaries of the green line (i.e., shock associated with CME2) and the sky-blue shading. The red line marks the start of the substorm (triggered by CME2) and the passage of a complex magnetic ejecta.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: The current population of observed polar Neptunes. We define polar Neptunes as planets with radii in the range R  p  = 1.5−7 R ⊕ or masses in the range M  p  = 10−50 M ⊕ and measured 3D stellar obliquities in the range Ψ = 80°−125°. The left panel shows this sample in planet radius–orbital period space, with the coloration according to the 3D stellar obliquity. The right panel shows their 3D stellar obliquities, Ψ, vs. the stellar effective temperature. The data are compiled from TEPCat (J. Southworth 2011) and originally from G. Á. Bakos et al. (2010), R. Sanchis-Ojeda & J. N. Winn (2011), A. Vanderburg et al. (2016), D. R. Anderson et al. (2017), F. Dai & J. N. Winn (2017), S. W. Yee et al. (2018), M. Hjorth et al. (2019), S. Dalal et al. (2019), V. Bourrier et al. (2021), G. Stefànsson et al. (2022), P. F. L. Maxted et al. (2022), and V. Bourrier et al. (2022, 2023). Note that there are several additional planets that have ∣λ∣ values suggestive of polar orbits, but they do not yet have constrained Ψ values. These planets include WASP-156 b (﹩\lambda ={105.7}_{-14.4}^{+14.0}{^\circ} ﹩; O. D. S. Demangeon et al. 2018; V. Bourrier et al. 2023), HATS-38 b (﹩\lambda =-{108}_{-16}^{+11}{^\circ} ﹩; A. Jordán et al. 2020; J. I. Espinoza-Retamal et al. 2024), and WASP-139 b (﹩\lambda =-{85.6}_{-4.2}^{+7.7}{^\circ} ﹩; C. Hellier et al. 2017; J. I. Espinoza-Retamal 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: Panels (a)–(e) are composite images, merging SDO/AIA 304 Å with SOHO/LASCO-C2 coronagraph images, revealing the dynamic interaction between CME1 and CME2. Arrows in panel (c) mark the brightness and reconnection between CME1 and CME2, while in panel (e) the arrows illustrate the bright core of CME2. The image at panel (f) is coronagraph SOHO/LASCO C3 with FOV extending to 32 R ⊙ for CME1 and CME2 together. Panels (g)–(i) are Solar pictures acquired on 2012 January 19 from the STEREO Ahead COR2 observations.
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: Left panel: first-order fit of the height–time data extracted from the SOHO/LASCO CME catalog of the CMEs that occurred on 2012 January 19, between 09:48 and 16:12 UT. Right panel: show the speed profiles of the CMEs as they propagate via the heliosphere. The CMEs are accelerating in LASCO FOV.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Schematic of the disk-driven resonance theory for the origins of polar Neptunes. The starting configuration (left) consists of a star with an approximately coplanar inner Neptune, outer cold Jupiter, and transition disk. The nodal precession of the outer planet is initially faster than that of the inner planet due to the presence of the disk, but as the disk mass decays, eventually a secular inclination resonance is encountered where the nodal precession rates of the two planets are equal. The inner Neptune’s inclination then increases, as does the eccentricity in some cases. The inner Neptune is left in a highly misaligned state that is often polar (right).
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: The top panels present running difference images from SDO/AIA 304 Å and SOHO/LASCO-C2 coronagraph, illustrating the dynamic interaction among the three CMEs. The middle panels are images of 195 Å SECCHI / EUVI, which are overlaid on STEREO B/COR1 coronagraph images. In the bottom panels, the interaction is further captured in images from SOHO/LASCO C3.
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: (a)–(c) Composite images of the CMEs and GCS wireframe (blue) showing the reconstructed Images. (d)–(f) shows estimated 3D velocities for each reconstructed CME.
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: The six panels show the spatial variability of NO volume emission rates monitored by SABER V2.0 during the impact of the first CME and resulting traveling ionospheric disturbance.
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: Composite gri image of SN 2022crv in NGC 3054 obtained with the Las Cumbres Observatory on 2022 March 4. The position of SN 2022crv is indicated by white tick marks.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Mass distribution for our initial sample corrected by the ﹩1/{V}_{\max }﹩ volume.
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 right: multiband light curves of SN 2022crv with respect to the time of V-band maximum brightness (JD 2,459,645.42). The marker size is larger than the uncertainties. The DLT40 Open filter light curve is calibrated to the r band. Upper left: a zoom around a few days before and after the discovery. Only the Open- and o-band light curves are plotted here to show the constraint on the explosion epoch. The last nondetection and the earliest detection are marked by the magenta vertical dashed line and blue vertical dashed line, respectively. The black vertical line marks when the multiband follow-up observations began. Bottom: the absolute V-band light curve of SN 2022crv compared with that of other SESNe. The multiband photometry of SN 2022crv is available in machine readable format as 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: Color evolution of SN 2022crv, after correcting for a total color excess of E(B − V) = 0.21 mag. The color templates are from M. D. Stritzinger et al. (2018). A sample of SNe Ib/IIb after correcting with the published reddening estimates is also plotted. In addition, the B − V color evolution is compared with the SNe Ib color evolution models by S.-C. Yoon et al. (2019) with various degrees of 56Ni (indicated by f  m ). SN 2022crv is more consistent with the f  m  = 0.15/0.3 model, suggesting relatively weak 56Ni mixing in the ejecta (see Section 4).
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: Velocity evolution of Hα, He I, Fe II, and feature A (see Section 5.3). The epoch of the explosion is marked with the vertical dashed line. The velocity of feature A is calculated assuming it is from C I λ1.0693 μm, Mg I λ1.0927 μm, Fe II λ1.05 μm, S I λ1.0457 μm, and Sr I λ1.0327 μm, and is shown with the plus symbol. The velocity of Hα shows a rapid drop after the ﹩{V}_{\max }﹩. As discussed in Section 6.1, the 6200 Å feature is likely dominated by Si II after ﹩{V}_{\max }﹩, so this drop does not reliably reflect the velocity evolution of the Hα line.
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: The optical spectroscopic evolution of SN 2022crv from the photospheric phase to the early nebular phase. The phase is measured from the dates of explosion and V-band maximum. 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: The nebular phase spectroscopic evolution of SN 2022crv. Phase is measured from the dates of the explosion and V-band maximum brightness. All spectra shown here are rebinned with a second-order Savitzky–Golay filter with a window size of 11 Å. 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: Top: a high-resolution spectrum taken with LRIS 50.3 days after the maximum light showing the Na I D lines from the host galaxy and the Milky Way. The continuum is fit with a fourth-order polynomial function. Bottom: the continuum-normalized spectrum. The Na I D lines are fitted with Gaussian functions using an MCMC routine.
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: Top: bolometric light curve of SN 2022crv compared with other SNe Ib/IIb. The unfilled points represent the bolometric light curve from the blackbody fit. Bottom: The evolution of temperature and radius of SN 2022crv derived from the blackbody fit.