adsabs/AstroCLIMB huggingface dataset:
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Upper panel: composite model (orange shaded region) between 13.4 and 15.5 μm compared to the Sz 114 JWST-MIRI spectrum (black). Lower panel: individual best fits to water, C2H2, HCN, and CO2.
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Sketch of the inner disk C/O ratio evolution with time. Substructures, depending on their locations and depths, can slow down the inward drift of icy pebbles. The time at which the C/O ratio starts to increase indicates the depletion time of the inner water-rich phase and depends on several factors, including stellar mass, initial disk size, mass, viscosity, and the presence and depth of substructures. Model predictions for disks with substructures around solar-type stars can be found in Kalyaan et al. (2023). Models for disks without substructures around stars of different masses are presented in Mah et al. (2023).
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: [Ne II] vs. accretion luminosities for the sample of late M-type (Pascucci et al. 2013) and disks around earlier-type stars (Banzatti et al. 2020). For the latter sample, [Ne II] fluxes are collected from Güdel et al. (2010) and Rigliaco et al. (2015).
Paper: Water-rich Disks around Late M Stars Unveiled: Exploring the Remarkable Case of Sz 114
Authors: Chengyan Xie, Ilaria Pascucci, Feng Long, Klaus M. Pontoppidan, Andrea Banzatti, Anusha Kalyaan, Colette Salyk, Yao Liu, Joan R. Najita, Paola Pinilla, Nicole Arulanantham, Gregory J. Herczeg, John Carr, Edwin A. Bergin, Nicholas P. Ballering, Sebastiaan Krijt, Geoffrey A. Blake, Ke Zhang, Karin I. Öberg, Joel D. Green
Figure caption: Corner plot of our hot water models as an example of our fitting. The vertical dashed lines indicate the 1σ of each parameter as the middle 68% of the accepted models. We can see the degeneracy between the three parameters from the shape of the distribution.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: Standard deviation map of CH3CN J = 12 − 11 peak brightness temperature for K transitions 2 to 4. Gray contours show the continuum emission at the same levels as in Figure 1, and the green triangles indicate the continuum peaks. The beam size ellipse is shown in the lower left corner.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: Example spectra of CH3OH ﹩{J}_{{K}_{a},{K}_{c}}={18}_{\mathrm{3,15}}-{17}_{\mathrm{4,14}}\,A,{v}_{t}=0﹩ toward different positions. Note that some lines are skewed and/or not necessarily Gaussian.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: ALMA 1.3 mm continuum emission of the G336.01–0.82 region. The map in (a) is centered in ALMA 1 and has radius of 8″, while in (b) a zoom-in view of the structures within 3″ is presented.
Paper: Are There Terrestrial Planets Lurking in the Outer Solar System?
Authors: Amir Siraj
Figure caption: Lower panel: cumulative fraction of captured free-floating planets as a function of apparent visual magnitude for Earth-, Venus-, Mars-, and Mercury-size planets. Upper panel: expected number of planets as a function of apparent visual magnitude, adopting a nominal albedo of 0.2.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: CH3OH ﹩{J}_{{K}_{a},{K}_{c}}={18}_{\mathrm{3,15}}-{17}_{\mathrm{4,14}}\,A,{v}_{t}=0﹩ pv maps. (a) The pv map following the gray line in Figure 2(a), i.e., perpendicular to the outflow/rotation axis (PA = 125°) and a slit width of 0.″1. The dotted green lines show the offset of the continuum sources ALMA1-WEST (left) and ALMA1-EAST (right). (b) The pv map of the northern spiral-like feature following the blue line in Figure 2(a) and a slit width of 0.″05. Zero offset corresponds to ALMA1-WEST. (c) The pv map of the southern spiral-like feature following the red line in Figure 2(a) and a slit width of 0.″05. Gray contour levels are −6, −3, 3, 6, 12, and 24 × σ with σ = 1.2 mJy beam−1. The blue contours in (a) are from an IRE model (see Section 4.1) at the same levels as the data relative to the peak, while the blue lines in (b) and (c) correspond to linear fits to data over 10σ. Zero offset corresponds to ALMA1-EAST. The dashed green line correspond to the systemic velocity v LSR = −47.2 km s−1.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: CH3OH ﹩{J}_{{K}_{a},{K}_{c}}={18}_{\mathrm{3,15}}-{17}_{\mathrm{4,14}}\,A,{v}_{t}=0﹩ moment maps. (a) Zeroth-order moment map. The blue and red lines mark the position of the north and south spiral-like features, respectively. The arrow marks the direction of the pv map in Figure 3(a) and corresponds to the line crossing all three continuum structures (PA = 125°). (b) First-order moment map. (c) Second-order moment map. The continuum is shown in contours with the same levels as in Figure 1, and the continuum peaks are marked with green triangles. The beam size ellipse is shown in the lower left corner.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: ALMA maps of G336.01–0.82. (a) Continuum map at 1.3 mm. The position of the three local continuum peaks is indicated by the green labeled triangles. The contour levels are −3, 5, 10, 20, 40, 80 × σ rms with σ rms = 55 μJy beam−1. (b) HC3N J = 24 − 23 l = 1f, v 7 = 1 zeroth moment map contours over the continuum map. The contours are 5, 8, 10, 15, 20, 25 × σ rms with σ rms = 11 mJy beam−1 km s−1. (c) SiO J = 5–4 blue- and redshifted, and the contour levels are 5, 6, 7 ... 12 × σ rms with σ rms = 7.7 mJy beam−1 km s−1. Velocity integration ranges with respect to the systemic velocity are annotated by the respective color. The beam size of the continuum map is shown in the lower left corner.
Paper: Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01–0.82
Authors: Fernando A. Olguin, Patricio Sanhueza, Huei-Ru Vivien Chen, Xing Lu, Yoko Oya, Qizhou Zhang, Adam Ginsburg, Kotomi Taniguchi, Shanghuo Li, Kaho Morii, Takeshi Sakai, Fumitaka Nakamura
Figure caption: Average peak brightness temperature from CH3CN J = 12 − 11 K transitions 2 to 4. The blue and red regions in (a) indicate where the properties in Section 4.2 are estimated and roughly follow the continuum 5σ level. Gray contours show the continuum emission from the combined data at the same levels as in Figure 1 but with σ rms = 54 μJy beam−1, and the green triangles indicate the continuum peaks. The beam size ellipse is shown in the lower left corner.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: HST/STIS UV-optical spectra of SN 2022wsp at +10 and +20 days compared with those of SN 2021yja at similar phases. All spectra have been dereddened. The SN 2022wsp flux density has been scaled by the same constant for both days such that the continuum level redward of 7000 Å matches that of SN 2021yja, demonstrating the dramatic evolution and variation in the UV, while showing general agreement at optical wavelengths. The spectra have also been shifted arbitrarily by a constant for easier comparison. The wavelength scale has been corrected to the rest frame using the recession velocity of the host galaxy. Balmer lines at an expansion velocity of v = 7500 km s−1 are marked by vertical dotted lines. The zero flux level of the top two spectra is indicated by the horizontal dashed line.(The data used to create this figure are available.)
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Zoomed-in view of the HST/STIS UV spectra of SN 2022wsp at +10 and +20 days for clearer comparison to Type IIP SNe 1999em (Baron et al. 2000) and 2021yja (Vasylyev et al. 2022). All spectra have been dereddened and are in units of 1 × 10−14 erg s−1 cm−2 Å−1. The spectra have the same scaling with the exception of SN 1999em, which was scaled by a factor of 0.5. From top to bottom, the flux density spectra have been offset vertically by 4.4, 3.5, 2.7, 1.2, 0.8 (×10−14 erg s−1 cm−2 Å−1); the zero-points are indicated by horizontal dashed lines.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption:  TARDIS fits to the HST STIS UV-optical spectra of SN 2022wsp at days +10 (top) and +20 (bottom). The best-fit parameters are presented above the top panel. The embedded subpanels at upper right present a zoomed-in view of the Mg II λ2798 feature. The gray-shaded areas mark interstellar absorption lines.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Temporal evolution of the photospheric temperature T ph (left) and photospheric velocity v ph (right) of SN 2022wsp obtained from the TARDIS fit to its days +10 (T ph=10,900 K, v ph = 8500 km s−1) and +20 (T ph=7700 K, v ph = 7500 km s−1) spectra compared to those of SNe 1999em, 2005cs, 2006bp, and 2021yja (Dessart et al. 2008, D08; Vogl et al. 2019, V19; Vasylyev et al. 2022). Vertical dashed line indicates the velocity at days +15, v d15, for comparison purposes.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Gaussian-convolved spectrum of SN 2022wsp (σ = 2500 km s−1; green) compared to observed SN 2021yja (blue) and SN 2022wsp (orange) spectra. Wavelength range is zoomed in on the Mg II profile. The convolved spectrum is blueshifted by 1250 km s−1 to match the spectral features with SN 2021yja. All spectra are dereddened.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption:  TARDIS fits to the HST STIS UV-optical spectra of SN 2022wsp at days +10 (top) and +20 (bottom) for varied T ph (all other parameters fixed). The two temperature deviations from the best-fit value (turquoise) on day +10 (T ph,best = 10,900 K) and day +20 (T ph,best=7700 K) are represented as T ph,best − 500 K (blue) and T ph,best + 500 K (red). The black curve represents observational data. Insets provide a detailed view of specific wavelength regions for easier comparison.
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Same as Figure A2 but instead varying the density-profile index n relative to the best-fit model n best = 24(16) on days +10(20). Density-profile variations are n best − 3 (blue) and n best (turquoise).
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Same as Figure A2 but instead varying the metallicity Z for values 0.5 Z ⊙ (blue), 1.0 Z ⊙ (turquoise), and 2.0 Z ⊙ (red).
Paper: Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
Authors: Sergiy S. Vasylyev, Christian Vogl, Yi Yang, 轶 杨, Alexei V. Filippenko, Thomas G. Brink, Peter J. Brown, Thomas Matheson, Maryam Modjaz, Avishay Gal-Yam, Paolo A. Mazzali, Thomas de Jaeger, Kishore C. Patra, Gabrielle E. Stewart
Figure caption: Same as Figure A2 but instead varying the photospheric velocity relative to the best-fit model v ph,best = 8500(7500) km s−1 at day +10 (20). The two photospheric velocity variations are 0.9v ph,best (blue) and 1.1v ph,best (red).
Paper: Observing Planetesimal Formation under Streaming Instability in the Rings of HD 163296
Authors: F. Zagaria, C. J. Clarke, R. A. Booth, S. Facchini, G. P. Rosotti
Figure caption: Top panel: maximum grain sizes compatible with the gas surface density estimate of Booth et al. (2019) and the upper limit on disk turbulence of Flaherty et al. (2017) for different dust compositions (see Appendix B of Birnstiel et al. 2018) in R67 (violet) and R100 (purple). The results (best-fit and 1σ spread) of Guidi et al. (2022) are shown as dots and shaded regions of the same color. Bottom panel: dust surface density estimates based on the best-fit of Guidi et al. (2022) in the optically thin limit.
Paper: Observing Planetesimal Formation under Streaming Instability in the Rings of HD 163296
Authors: F. Zagaria, C. J. Clarke, R. A. Booth, S. Facchini, G. P. Rosotti
Figure caption: Dust-to-gas ratio and Stokes number of the 67 au (violet) and 100 au (purple) rings of HD 163296 plotted against the threshold for particle clumping in laminar disks (α turb = 0) of Li & Youdin (2021). Squares display the values determined using the gas surface densities from Table 1, while circles show those computed from the gas mass measured by (Booth et al. 2019; see Table 2). The 100 au ring is prone to particle clumping under SI.
Paper: Observing Planetesimal Formation under Streaming Instability in the Rings of HD 163296
Authors: F. Zagaria, C. J. Clarke, R. A. Booth, S. Facchini, G. P. Rosotti
Figure caption: Same as Figure 1 but showing the threshold for particle clumping of Li & Youdin (2021) corrected for an isotropic turbulence level of α turb = 3.32 × 10−4. Both rings are stable against SI-driven particle clumping. However, we stress that turbulence is nonisotropic in R67 and R100, which leads to less stringent conditions for particle clumping.
Paper: Observing Planetesimal Formation under Streaming Instability in the Rings of HD 163296
Authors: F. Zagaria, C. J. Clarke, R. A. Booth, S. Facchini, G. P. Rosotti
Figure caption: Comparison of the dust-to-gas surface density ratio and Stokes number for different compositions (color-coded) with the threshold for particle clumping of Li & Youdin (2021) in the laminar case. Our results that the 100 au ring is undergoing particle clumping under SI is consistent with different assumptions on grain mixtures.
Paper: The Effect of the Parametric Decay Instability on the Morphology of Coronal Type III Radio Bursts
Authors: Chaitanya Prasad Sishtla, Immanuel Christopher Jebaraj, Jens Pomoell, Norbert Magyar, Marc Pulupa, Emilia Kilpua, Stuart D. Bale
Figure caption: Example dynamic radio spectra produced from the measurements of FIELDS/RFS onboard PSP during encounter 9 (2021 November 22). The probe was approximately 17 R ⊙ during the time intervals at which these measurements were made. A few examples of the “structured” type III radio bursts are indicated in the top panel. The local plasma frequency at the spacecraft (f pe) is also marked in both spectra.
Paper: The Effect of the Parametric Decay Instability on the Morphology of Coronal Type III Radio Bursts
Authors: Chaitanya Prasad Sishtla, Immanuel Christopher Jebaraj, Jens Pomoell, Norbert Magyar, Marc Pulupa, Emilia Kilpua, Stuart D. Bale
Figure caption: The spatiotemporal dependence of the (a) local plasma frequency in the solar wind, and (b) the associated simulated dynamic spectrum for a radiation source injected at t = 1000 minutes is shown. The path of the radiation source is annotated in (a). Subsequently, panels (c) and (d) present the local plasma frequency annotated with the path of a beamlet and the associated dynamic spectrum. In panel (d) the dynamic spectrum is colored based on the 5 minute averaged density fluctuations encountered by the beamlet. Similar to panels (a) and (b), panels (e) and (f) present the modeled emission for a radiation source but in a solar wind injected with Alfvén waves with frequencies 1, 2, and 3 mHz. Panels (g) and (h) present the modeled emissions for a similar beamlet as in panels (c) and (d) but in a solar wind injected with the Alfvén waves of three different frequencies.
Paper: The Effect of the Parametric Decay Instability on the Morphology of Coronal Type III Radio Bursts
Authors: Chaitanya Prasad Sishtla, Immanuel Christopher Jebaraj, Jens Pomoell, Norbert Magyar, Marc Pulupa, Emilia Kilpua, Stuart D. Bale
Figure caption: Dynamical evolution of the solar wind plasma along the flux tube. In every panel, each column represents the quantity (indicated with the color bar) at the given time along the flux tube. The panels show the parameters (a) v  ϕ , (b) v  θ , (c) v  r , and (d) v  r /v  a  for the case where a 1 mHz Alfvén wave is continually injected starting at t = 0. In addition, the density fluctuations defined as δ ρ/ρ 0, where ρ 0 is the time-averaged density are presented for different averaging intervals of (e) 0.5 minutes, (f) 1.25 minutes, (g) 2.5 minutes, and (h) 5 minutes.
Paper: Discovery of the Closest Ultra-stripped Supernova: SN 2021agco in UGC 3855
Authors: Shengyu Yan, Xiaofeng Wang, Xing Gao, Jujia Zhang, Alexei V. Filippenko, Thomas G. Brink, Jun Mo, Weili Lin, Danfeng Xiang, Xiaoran Ma, Fangzhou Guo, Lina Tomasella, Stefano Benetti, Yongzhi Cai, Enrico Cappellaro, Zhihao Chen, Zhitong Li, Andrea Pastorello, Tianmeng Zhang
Figure caption: Comparisons of absolute g- and r-band light curves, g − r color, and rise time of SN 2021agco with other SESNe. Top panels: the left panel presents the SN 2021agco light curves in r (circles), o (crosses), and clear band (hollow triangles) with E(B − V) = 0.11 compared with other SESNe in r, while the right panels are in g. The epochs correspond to the r-band peaks. Bottom-left panel: SN 2021agco g − r color evolution compared with other SESNe. Bottom-right panel: the r-band peak luminosity vs. the rise time (t rise). Comparisons of the decay timescale are shown in Appendix B.2 (Figure 8). The objects including fast-evolving Type I transients SN 2002bj (Poznanski et al. 2010), SN 2005ek (Drout et al. 2013), SN 2010X (Kasliwal et al. 2010), SN 2018kzr (McBrien et al. 2019), and SN 2019bkc (Chen et al. 2020); Ca-rich transients iPTF16hgs (De et al. 2018a), PTF 09dav (Sullivan et al. 2011), and PTF10iuv (Kasliwal et al. 2012); FBOTs KSN2015K (Rest et al. 2018), iPTF2016asu (Whitesides et al. 2017), AT 2018cow (Perley et al. 2018; Prentice et al. 2018), SN 2018gep (Ho et al. 2019), and ZTF 18abvkwla (Ho et al. 2020); and USSN iPTF14gqr (De et al. 2018b) and SN 2019dge (Yao et al. 2020).
Paper: Discovery of the Closest Ultra-stripped Supernova: SN 2021agco in UGC 3855
Authors: Shengyu Yan, Xiaofeng Wang, Xing Gao, Jujia Zhang, Alexei V. Filippenko, Thomas G. Brink, Jun Mo, Weili Lin, Danfeng Xiang, Xiaoran Ma, Fangzhou Guo, Lina Tomasella, Stefano Benetti, Yongzhi Cai, Enrico Cappellaro, Zhihao Chen, Zhitong Li, Andrea Pastorello, Tianmeng Zhang
Figure caption: Panel (a): t ≈ + 1.0 and +2.0 days spectra of SN 2021agco (red lines) compared with the peak spectra of other SESNe (black lines). Strong emission lines from the host galaxy are marked with gray lines. Panel (b): spectra at +5.5 and +8.9 days post peak compared with SN 2005bf at +6 days and SN 2019dge at +11.8 days. Panel (c): SN 2021agco spectrum at +25.9 days compared with other helium-rich SNe. The flux density is plotted on a linear scale and adjusted for better display. The spectra of SN 2021agco and iPTF16hgs have been rebinned to improve the spectral quality. Panel (d): the spectra taken at +5.5 and +8.9 days (red lines) compared with the synthetic spectra (black lines at the bottom). The best-fit SYN++ model spectra together with absorption lines due to different ions are shown with black lines.