adsabs/AstroCLIMB huggingface dataset:
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: gcroJHKs-band light curves of SN 2023xgo. Filled circles represent JHKs-band magnitudes from kSIRIUS. Diamonds indicate g- and r-band magnitudes from ZTF. Asterisks denote o- and c-band magnitudes from ATLAS. The JHKs magnitudes are in the Vega system, while the groc-band magnitudes are in the AB system.
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: Spectra of SN 2023xgo at t = 4.4 and 31.4 days (C. Balcon 2023; J. Sollerman et al. 2023). The wavelength has been corrected to its rest wavelength using a redshift of z = 0.01325. The emission lines detected in the spectra are denoted by the vertical lines.
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: Spectral energy distributions (SEDs) at t = 16.8, 26.8, and 50.0 days. The blue lines show the hot-component blackbody model. The red lines represent the dust model, which explains the NIR excess and is present from t = 16.8 days. The black lines represent the combined model of the hot component and the dust model.
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: The H − Ks, J − Ks, and J − H color evolution of SN 2023xgo is shown, compared with those of SNe 2006jc, 2010al, OGLE2012SN 006, and SN 2007gr. The color coding is the same as in Figure 3.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: Left: FDF of the single polarized detection of CHIME J0630+25 showing linear polarized intensity as a function of the trial Faraday depths, ϕ. Inset plot highlights the FDF peak near an RM ∼ −350 rad m−2. Right: DM–∣RM∣ distribution of the Galactic pulsar sample (blue points; ATNF Catalog) vs. the equivalent measurement from CHIME J0630+25 (red star). Diagonal gray lines indicate different magnetic field strengths (0.01,0.1,1,10,100 μG) determined from the relation, ﹩{B}_{\parallel }=1.23\frac{| {\rm{RM}}| }{{\rm{DM}}}\ \mu {\rm{G}}﹩.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption:  ﹩P-\dot{P}﹩ diagram. 1E161348–5055, a central compact object that shows evidence of magnetar-like emission, is shown with a gray star (A. D’Aì et al. 2016). The longest-period pulsars PSR J2050+5854 and LPT PSR J0901–4046 are shown by the colored dots and labeled as such. The gray-shaded region shows the death valley for coherent pulsed radio emission. The black dashed line corresponds to a pure dipole, dotted lines to a twisted dipole, and solid lines to a twisted multipole configuration (K. Chen & M. Ruderman 1993; B. Zhang et al. 2000). The blue dashed lines correspond to lines of constant age, and the gray solid lines correspond to lines of constant magnetic field. All downward-facing arrows correspond to upper limits and are at the 1σ level.