adsabs/AstroCLIMB huggingface dataset:
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: Mass–radius–distance (top panels) and envelope–radius–distance (bottom panels) parameter spaces for the deuterium-enhanced atmosphere in our grid of simulations shown in Figure 2. In the parameter space from (R  p , d) ≈ (2.4 R ⊕, 0.1 au) to (1.7 R ⊕, 0.4 au), the data points increase with time, meaning more deuterium-enhanced sub-Neptunes along the upper edge of the radius valley during the photoevaporation evolution. As illustrated in the bottom panels, the planets with initial low envelope fractions, i.e., f env = 0.001 and 0.003, can become deuterium-enhanced, which is expected from Figure 1. The top panels show that more massive planets, i.e., M  p  = 10 and 15 M ⊕, with low f env can become deuterium-enhanced as the orbital distance decreases.
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: Mass–radius–distance (top panels) and envelope–radius–distance (bottom panels) parameter spaces and time frames for the appearance of bare rocky cores (denoted by color-coded crosses) in our grid of simulations without the H–D–He fractionation. The bare cores of the same d and R  p  are plotted side by side to distinguish them. Despite no fractionations, the sub-Neptunes shown by gray dots are identical to those in Figure 2. The sub-Neptunes in the d–R  d  parameter space shown by green dots survive up to t = 7.5 Gyr in the grid of simulations without fractionations, whereas they are disregarded from Figure 2 due to a radius anomaly in the grid of simulations with fractionations. The parameter spaces of bare cores become wider with time, meaning more sub-Neptunes evolving to bare cores over time.
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: The D/H ratio of giant and icy planets in the solar system (J: Jupiter, S: Saturn, U: Uranus, and N: Neptune), along with the simulated ratio of the photoevaporating sub-Neptunes along the upper edge of the radius valley. The D/H values of Earth’s ocean and the protosolar nebula are shown by blue and gray horizontal lines, respectively. Analogous to the helium-enhanced planets due to atmospheric escape (Malsky et al. 2023), the planets along the upper boundary of the radius valley generally exhibit the largest D/H value in their thin atmospheres (see Figure 2). The simulated D/H value along the upper radius valley only provides the lower limit.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: A time series of the extinction-corrected UV and optical spectra of SN 2022acko (black) and the well-matched CMFGEN models (pink; scaled as described in Section 5.1). The phase (in days) of each spectrum is given on the left for the UV observations, in the center for the optical observations, and on the right for the models. The day 19 spectra (observed and scaled model) are at their true flux, while the day 7 spectra are shifted by 2 × 10−15 erg cm−2 s−1 Å−1, the day 6 spectra are shifted by 5 × 10−15 erg cm−2 s−1 Å−1, and the day 5 spectra are shifted by 8 × 10−15 erg cm−2 s−1 Å−1. The model spectra shown in this figure are available as the data behind the figure.(The data used to create this figure are available.)
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: SN 2022acko (black) in the context of the UV evolution of Type IIP supernovae, showing the diversity of UV spectra. Swift and HST NUV spectra of SN 2021yja (pink; Vasylyev et al. 2022) span 4–21 days postexplosion. HST NUV spectra of SN 2022wsp (maroon) are shown for days 10 and 20 (Vasylyev et al. 2023). A Swift spectrum of the LLSN SN 2005cs (teal; M. Rowe 2023, in preparation) is shown as well. SN 2022acko and SN 1999em (blue; Baron et al. 2000) are the only Type IIP/L supernovae with FUV spectra, with the first epochs of SN 2022acko observed significantly earlier than SN 1999em, resulting in strong FUV features. Iron line blanketing is already significantly suppressing the FUV flux by day ∼12 in the SN 1999em spectrum.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The observed fractional throughput (black) as a function of shortest wavelength observed for day 5 (dot), day 7 (circle), and day 19 (triangle) spectra. Plotted in pink in the fractional flux from the best-fit absorbed blackbody spectrum calculated using Equation (1) and with the same symbols representing the different epochs as were used for the observed flux. At all epochs, the absorbed blackbody approximation yields a fractional flux within 7% of the true value. The cutoff wavelengths that were used for the filters given in Table 5 are shown as vertical lines and labeled in the plot.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The absolute and extinction-corrected apparent magnitude optical and UV light curves of SN 2022acko. The left panel shows the first 7 days of evolution, highlighting the tightly constraining nondetections within 24 hr of discovery and high-cadence follow-up observations obtained immediately by the DLT40 and ATLAS surveys. No offset is applied to these filters in either panel. The DLT40 open filter is calibrated to the r band while the ATLAS o filter is similar to the r+i band (5600–8200 Å). The right panel shows the full multiband light curve, including the UV evolution. Ticks at the bottom of each panel mark epochs of spectroscopic observations with optical spectra marked in light blue and HST UV spectra shown in pink. The photometry shown this figure is available as the data behind the figure.(The data used to create this figure are available.)
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The identification of species present in the day 5 HST/STIS UV spectrum of SN 2022acko. Top: the UV spectrum of SN 2022acko (black) with the total CMFGEN low-energy model overplotted in pink. The CMFGEN continuum flux is shown in blue, demonstrating the strong deviation of the observed spectrum from a blackbody. Although this is a complicated region, a few fairly isolated lines are identified below the spectrum. Bottom: the contribution of the most prominent ions, grouped by species, to the full spectrum. The model spectra of individual ions in this figure are available as the data behind the figure.(The data used to create this figure are available.)
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The photospheric evolution of SN 2022acko compared to those of SN 1999em (Dessart & Hillier 2006), SN 2005cs, and SN 2006bp (Dessart et al. 2008). The photospheric temperature (left), radius (middle), and velocity (right) fall between the derived parameters for SN 1999em, SN 2005cs, and SN 2006bp, indicating that this is not an unusual event.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The V-band slope at 50 days vs. V-band peak absolute magnitude for a sample of Type II supernovae (SNDAVIS database and Valenti et al. 2016), showing that SN 2022acko (black star) is a low-luminosity supernova, similar to SN 2005cs (blue circle), SN 2018lab (mustard circle; Pearson et al. 2023), SN 2021gmj (green circle; N. Meza 2023, in preparation), and SN 2012A (magenta circle). The slope at 50 days lies between that of SN 2005cs, SN 2018lab, SN 2021gmj, and SN 2012A. We include other supernovae with important UV data sets: SN 1999em and SN 2021yja.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The optical evolution of SN 2022acko (black) is very similar to the LLSNe SN 2005cs (pink; Pastorello et al. 2006, 2009) and transitional luminosity SN 2012A (blue; Tomasella et al. 2013). The similarity of the spectra can be seen here at both   ∼ 8 and ∼50 days postexplosion, with SN 2022acko falling between SN 2005cs and SN 2012A in terms of line widths (ejecta velocity).
Paper: Evidence of a Massive Stellar Disruption in the X-Ray Spectrum of ASASSN-14li
Authors: Jon M. Miller, Brenna Mockler, Enrico Ramirez-Ruiz, Paul A. Draghis, Jeremy J. Drake, John Raymond, Mark T. Reynolds, Xin Xiang, Sol Bin Yun, Abderahmen Zoghbi
Figure caption: RGS1 (black) and RGS2 (gray) spectra of ASASSN-14li from the longest XMM-Newton observation of this TDE. The wavelength scale is shifted to the frame of the host galaxy. The model in blue (XMMs in Table 1) represents the best pion photoionized absorption model with solar abundances. The H-like N VII resonance line at 24.78 Å and the He-like N VI resonance line at 28.78 Å are underpredicted, while the H-like C VI resonance line at 33.73 Å is overpredicted. The model in red (XMMt in Table 1) shows the best absorption model when the abundances of carbon and nitrogen are allowed to vary. An enhanced N abundance, potentially as high as 100 times solar, provides a better fit to the N lines. Similarly, the data require that the C abundance is at most 0.4 times solar, giving [N/C] ≥ 2.4. Please see the text and Table 1 for additional details.
Paper: Evidence of a Massive Stellar Disruption in the X-Ray Spectrum of ASASSN-14li
Authors: Jon M. Miller, Brenna Mockler, Enrico Ramirez-Ruiz, Paul A. Draghis, Jeremy J. Drake, John Raymond, Mark T. Reynolds, Xin Xiang, Sol Bin Yun, Abderahmen Zoghbi
Figure caption: Narrow, 2.5 Å slices of the XMM-Newton spectra of ASASSN-14li shown in Figure 1. The RGS1 spectrum is shown in black; the RGS2 spectrum in gray. Both spectra are shifted to the host frame. The model in blue is XMMs with solar abundances; the model in red is XMMt with thawed N and C abundances, giving [N/C] ≥ 2.4. The left panel centers the H-like N VII line at 24.78 Å, the middle panel centers the He-like N VI line at 28.78 Å, and the right panel centers the H-like C VI line at 33.73 Å.
Paper: First Observation of a Double-peaked O I Emission in the Near-infrared Spectrum of an Active Galaxy
Authors: Denimara Dias dos Santos, Alberto Rodríguez-Ardila, Swayamtrupta Panda, Murilo Marinello
Figure caption: NIR spectra of the III Zw 002 in rest wavelength, observed with GEMINI-N/GNIRS on 2021 July 28. Here we show the spectral region of J and K bands, respectively, covering 0.7–1.3 μm (upper panel) and 1.7–2.3 μm (lower panel). We also mark the most notable emission lines and in boldface the emission lines exhibiting double-peaked features. The background atmospheric transmission filter is represented in gray.
Paper: First Observation of a Double-peaked O I Emission in the Near-infrared Spectrum of an Active Galaxy
Authors: Denimara Dias dos Santos, Alberto Rodríguez-Ardila, Swayamtrupta Panda, Murilo Marinello
Figure caption: Paα and O I emission line fits. Left: observed profile for Paα (black solid line), fitted double-peaked component (red solid line), and residuals in the gray line. The dotted and dashed red lines are narrow and broad Gaussian components, respectively. Right: fit of the O I, where the colors have the same meaning for the disk and broad Gaussian component.
Paper: First Observation of a Double-peaked O I Emission in the Near-infrared Spectrum of an Active Galaxy
Authors: Denimara Dias dos Santos, Alberto Rodríguez-Ardila, Swayamtrupta Panda, Murilo Marinello
Figure caption: Overlapping double-peak profile for Paschen α in the solid black line, and O I in the dotted gray line. We subtract the narrow component of Paschen α to compare the profiles.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: (a) Measurement of individual emission lines (gray histograms) with either a single (black lines) or a double (blue and red lines) Gaussian function, after subtracting a best-fit local, linear continuum. (b) PAH decomposition, after masking the emission lines, of the MIRI/MRS spectrum (gray solid line) with a multicomponent model (red solid line) consisting of a PAH template (green dashed line) and three dust continuum components (blue dashed lines), each represented by a modified blackbody (MBB), corrected for extinction. (c) PAH measurement from the residual PAH spectrum (gray solid line) using a series of Drude profiles (dashed curves) for the individual PAH features, which combine to produce the total model (red solid curve). The residual PAH spectrum was formed from subtracting the best-fit continuum components from the MRS spectrum. The gray stripes mark the regions masked because of emission lines.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: The distribution of (a) SFR and (b) SFE for the central region of NGC 7469. The black contours in panel (a) indicate the distribution of H2 content derived from the CO(1–0) emission line. The SFE is calculated based on the SFR and H2 content in panel (a). Panel (b) features a filled gray circle to indicate the angular resolution, a compass (with a rotation angle of 23°), and a scale bar; they are the same for the SFR and H2 maps in panel (a), and for all subsequent colored maps, unless specifically noted.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: Illustration of the MIRI/MRS coverage (white rectangle) of NGC 7469, with the NIRCam F335M image as background. The inset shows the distribution of 7.7 μm PAH emission to illustrate the circumnuclear starburst ring. The bright blob in the lower left corner is part of the companion galaxy IC 5283.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: The distribution of the Toomre Q parameter for the central region of NGC 7469, calculated from the CO observations. The filled gray ellipse in the bottom left corner indicates the synthesized beam of the CO map. Note that the distribution is sparse because the velocity and velocity dispersion of the CO line are available only for the pixels with sufficiently strong CO emission.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: A timeline of events from discovery through the end of HST observations for SN 2022acko. The bottom panel shows the DLT40 open filter light curve (open circles) and the ATLAS limits (orange triangles). Key moments in the timeline are marked on the light curve. The epochs at which optical spectra were obtained are shown as light blue lines at the bottom of the figure. We observed at least one optical spectrum concurrent with each HST visit. The top panel shows the details of activities executed in the first 3 days after explosion to enable the triggering of HST. If any one of these events was unable to occur or was delayed, we would not have been able to observe SN 2022acko in the FUV.
Paper: SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
Authors: K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, 一泽 董, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, Samuel Wyatt
Figure caption: The spectroscopic evolution of SN 2022acko in the optical. The phase of each spectrum, relative to the date of last nondetection, is marked on the right. Telluric features are marked at the top of the figure. The spectra shown in this figure are available as the data behind the figure.(The data used to create this figure are available.)