adsabs/AstroCLIMB huggingface dataset:
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Comparison of the cumulative probability distributions for solar wind at 1 au. Shown are the SWMF results for solar wind parameters driven by real (red) and synthetic (blue) magnetogram data for CRs (a) 1925, (b) 1957, (c) 1989, (d) 2021, (e) 2069, (f) 2086, (g) 2112, (h) 2151, and (i) 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Average RMSE of EUVI for (left) 171, (middle) 195, and (right) 284 Å.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: The position–velocity (PV) diagrams obtained from slicing the CO data cube along (top) and perpendicular to (bottom) the stellar kinematic PA. The black contours on the PV diagrams mark 3σ, 5σ, 10σ, 15σ, and 20σ levels, respectively. The left columns are contours of the CO moment0 map (green) on top of the HST F606W image. The green contour levels are logarithmically spaced from 13% to 90% of the peak CO moment0 flux. The small ellipse in the upper corner shows the beam, and the pink lines outline the slabs for the PV diagrams. The high-velocity blob marked by the red circle in the lower right PV diagram is suggestive of disturbed gas not following bulk gas motion, possibly outflowing gas moving away from us. The location of the circled blob is marked by a red star on the HST image on the left.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: The radio spectrum of IC 860 based on selected, public, wide-field radio surveys. The best-fit power-law model (with a spectral index of α = −0.15) is shown by the solid line. The dashed line illustrates the fit to a synchrotron self-absorption model typical of compact radio emission arising from an AGN. The radio spectral models follow the definitions from Patil et al. (2022). Further details on the radio surveys used in this analysis are provided in Table 2. The smaller panels show the selected cutout images (5﹩{}^{{\prime} }\times {5}^{{\prime} }﹩) from the radio surveys used in the spectral modeling, which demonstrate the highly compact nature of the radio source in IC 860.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Surface densities of the molecular gas mass and star formation rate compared to the Kennicutt–Schmidt star formation relation. We assume that the molecular gas and SF are cospatial, and use the radius of the CO gas distribution (1 kpc) to calculate the area of the gas and star formation regions. The data and the empirical relation from Kennicutt & De Los Reyes (2021) are plotted in black, while the estimations for IC 860 are plotted in color. The longer timescale SFRs (IR and UV + IR as indicators) are consistent with starburst on the relation, while the recent SFRs (Hα, Paα, and Ne as indicators) lie below the relation.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: The A V  extinction maps from spatially resolved SED fitting with HST data (Section 3.4.2). The mean errors for AV,birthcloud and AV,diffuseISM are 1.6 and 1.3, respectively. The sector marks the outflow cone region selected to constrain the hydrogen outflow mass (Section 4.5).
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: MIR color plot of IC 860 with AGN selection regions shaded in colors (Section 5.3). Although IC 860 does not fall in the AGN region, it is extremely close. As discussed in the text, IC 860 is actually a SF-AGN composite.
Paper: A Comparative L-dwarf Sample Exploring the Interplay between Atmospheric Assumptions and Data Properties
Authors: Eileen C. Gonzales, Ben Burningham, Jacqueline K. Faherty, Nikole K. Lewis, Channon Visscher, Mark Marley
Figure caption: Retrieved P-T profiles of the sample. For each P-T profile, the solid line indicates the median while the shaded region indicates the 1σ confidence interval. The gray bar indicates the approximate range of the photosphere for the comparison sample. (a) Spectral type comparison P-T profiles: J1526+2043 (purples) and J1416+1348A (black and red). While the cloudless model is the best fit for J1526+2043, we show the power-law deck-cloud model for comparison. (b) T eff comparison cloudy models: J1539−0502 (purple), GD 165B (pink), and J0539−0059 (blue) compared to J1416+1348A (black and red). Overplotted are the Sonora low-metallicity, log g = 5.0 (dotted) model profile (Marley et al. 2021) and the Saumon & Marley (2008) f sed = 2, log g = 5.0 (dotted–dashed) model profiles, which bracket the SED-derived and retrieval-derived effective temperatures (neon green and purple). The far right shows the location of the median cloud top (in purple, where the cloud is optically thick at τ = 1) and vertical distribution of the cloud (in blue shading, showing up to dashed line where the opacity drops to τ = 0.5) for J1416+1348A as a guide. The clouds for all comparative objects are in a similar location. (c) T eff comparison cloudless models: J1539−0520 (purple) and J0539−0059 (blue) compared to J1416+1348A in black and red. Overplotted are the Sonora solar (solid) and low-metallicity (dashed) model profiles, which bracket the SED-derived and retrieval-derived effective temperatures (neon green and purple).
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Density structure of the hydrogen-rich envelope of several models with nearly the same final helium core and envelope masses. Top: the structure is evaluated at the onset of pulsational activity (T  c  =  1.2 GK) for four models with helium core masses (not plotted) near 46.5 M ⊙ and hydrogen envelopes near 17 M ⊙, but different values of mixing-length parameters (α) and surface boundary pressures (P bound). Zero on the mass scale is the base of the hydrogen envelope. The models are TH102p25, TH102p45*, M105p6, and M106p75 in Table 3. Higher surface boundary pressure and greater mixing lengths lead to denser, more compact envelopes with smaller radii. Bottom: the density structures for models TH102p25 (red lines, α = 1, P bound = 100 dynes cm−2) and M105p6 (black lines, α = 2, P bound = 5000 dynes cm−2) evolve considerably following helium depletion (dashed–dotted lines) and pre-carbon ignition (T  c  =  0.5 GK; dashed lines). The solid lines show the structure at carbon depletion (T  c  =  1.2 GK) as in the top panel. In these two models, a surface convection zone eats deeper into the envelope as the core contracts, moving more matter to larger radii. Note surface density inversions in model TH102p25.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Top: ejected composition and terminal velocity for model M140p125. Bottom: approximate bolometric light curves for the six PISN models in Table 2 compared with observations (diamond symbols; Table 1). The velocity and composition of model M140p125 are typical of the five models that have some similarity to SN 1961V, although the velocity inferred for hydrogen lines in the spectrum would be slower for model TH140p0, which had no pre-SN wind mass loss. Models M140p25, M140p125, A155p2, and A160p2 were blue supergiants and had a more compact structure when they exploded. Models TH140p0 and TH140p125 were red supergiants with very low density hydrogen envelopes. Tails due to the decay of 56Co are apparent. None of the models resemble closely the observations of SN 1961V, which is why we favor pulsational pair models for SN 1961V as opposed to a true PISN.
Paper: A Comparative L-dwarf Sample Exploring the Interplay between Atmospheric Assumptions and Data Properties
Authors: Eileen C. Gonzales, Ben Burningham, Jacqueline K. Faherty, Nikole K. Lewis, Channon Visscher, Mark Marley
Figure caption: Distance-calibrated SEDs of J1416+1348A (dark blue) and comparative sources of similar T eff (J0539−0059, GD 165B, and J1539−0520 in grays) and of the same optical spectral type (J1526+2043 in light blue). All spectra were resampled to the same dispersion relation using a wavelength-dependent Gaussian convolution. The spectra are flux calibrated and scaled to the absolute magnitudes of the photometry shown. No normalization is applied.
Paper: Key Parameters Controlling the Photodesorption Yield in Interstellar CO Ice Analogs: The Influence of Ice Deposition Temperature and Thickness
Authors: Ni-En Sie, Yun-Ting Cho, Chao-Hui Huang, Guillermo M. Muñoz Caro, Li-Chieh Hsiao, Hsien-Chou Lin, Yu-Jung Chen
Figure caption: (a) L(T) and (b) Y(T) times R  A (T) as a function of deposition temperature.
Paper: A Comparative L-dwarf Sample Exploring the Interplay between Atmospheric Assumptions and Data Properties
Authors: Eileen C. Gonzales, Ben Burningham, Jacqueline K. Faherty, Nikole K. Lewis, Channon Visscher, Mark Marley
Figure caption: Retrieved P-T profile of GD 165B. The gray bar indicates the approximate range of the photosphere. Overplotted are the Saumon & Marley (2008) model profiles that bracket the SED- and retrieval-based T eff (magenta and neon green dot dashed, respectively), along with various cloud species condensation curves (colored dashed).
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Pulsing history of model TH102p25, a representative example of the class of single-event models. The central temperature (solid red line) and density (solid blue line) are shown as a function of time to core collapse. Six well-defined pulses happen in a space of 80 days. The last rise to a central temperature above 8 GK indicates collapse of a black hole. No outward shock is generated by this final event.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Misalignment angle, δ, resulting from the formation of the second BH in a BH+BH system, for a fixed pre-SN orbital period of P orb = 3.0 days and a kick velocity of w = 500 km s−1, as a function of the two kick angles: θ and ϕ. The mass of the collapsing star is assumed to be M He = 10.0 M ⊙ and it produces a BH of mass, M BH,2 = 8.0 M ⊙. The mass of the companion star, the first-born BH, is assumed to be M BH,1 = 12.0 M ⊙. The gray region to the left represents post-SN systems that are disrupted due to the SN, i.e., θ < θ crit = 105.°4. Above another critical angle, θ > θ retro = 145.°8, the post-SN orbits are always retrograde (δ > 90°, i.e., the newly formed BH is shot into an orbit such that the spin vector of the (old) first-born BH is pointing in the hemisphere opposite to that of the new orbital angular momentum vector). The blue lines represent values of ϕ between 0 and 90°, in steps of 10°.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Top: distribution of measured individual mean values of effective inspiral spins of 85 observed BH+BH merger events. Green and red colors indicate χ eff > 0 and χ eff < 0, respectively, and the arrow marks the average value, 〈χ eff〉 = 0.091. The distribution is clearly asymmetric and has a number of negative values. Central and bottom: inferred component masses of primary and secondary BHs (M 2 > 3.0 M ⊙) with average values stated. Data is taken from GWTC-3 (Abbott et al. 2022a).
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Effective spin, χ eff, as a function of kick velocity, w, and kick angle, θ (color-coded curves, red to blue with increasing θ), imparted on the second-born BH for the same 12 + 8 M ⊙ BH+BH system as in Figures 2–4. (The family of curves shifted to larger w values are for 59 + 16 M ⊙ BH+BH systems.) Panels (A)–(D) are for different pre-SN orbital periods, P orb,i, and BH component spins, χ 1,2. The little open black circle in panel (A) indicates (w, χ eff) = (500 km s−1, 0.0), where θ = θ retro = 145.°8.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Post-SN parameters calculated from SN conditions similar to those of Figures 2 and 3, except that in all cases here the second kick angle, ϕ = 60° is fixed and the kick velocity, w is a variable. Color coded (red to blue): misalignment angle, δ (top left); orbital period, P orb (top right); eccentricity, e (bottom left); and merger time, τ GW (bottom right), as a function of kick angle, θ and kick velocity, w. The systems above the black line have a first-born BH with a retrograde spin because of the kick tilting the orbit, δ > 90°.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Misalignment angle, δ (color coded; see vertical bar) as a function of the two kick angles, ϕ and θ. The pre-SN parameters are identical to those in Figure 2. The two angles θ crit = 105.°4 and θ retro = 145.°8, marked with arrows, are clearly noticeable (see also Figure 2).
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption:  12CO integrated intensity maps for eight of our sources. Molecular outflows can be seen emanating from the central protostellar source. A representative beam size and a scale bar showing 2000 au can be seen in the bottom left panel. The location of the submillimeter source is marked with a cyan plus sign.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: Left: cumulative dust mass distributions for disks around Class I and flat-spectrum protostars in young star-forming regions. Right: corresponding Gaussian distributions for the probability distribution functions of each region. Shading indicates the range of allowed fits.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: Stellar mass as a function of disk dust mass. A correlation is seen between the two quantities, but with a high degree of scatter, similarly to what was found in Law et al. (2017, Figure 5).
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: Multiband light curves of four SNe Icn. MJD and phases with respect to the estimated explosion dates are given, and photometry is given in apparent and absolute magnitudes. uvw2-, uvm2-, uvw1-, U-, B-, and V-band photometry is calibrated to Vega magnitudes, while other bands are calibrated to AB magnitudes. LCO photometry is marked by circles, ZTF photometry by squares, ATLAS photometry by pentagons, and Swift photometry by stars. For comparison, ugriz-band photometry from Gal-Yam et al. (2022) and Perley et al. (2022) is shown in lighter shaded diamonds. The photometry of all the objects except SN 2019jc has been template subtracted; as SN 2019jc is at the outskirts of its host galaxy, it should not suffer from significant host contamination. Dashed lines show the quadratic splines used to estimate the rise times and peak magnitudes of SN 2019jc, SN 2019hgp, and SN 2021ckj.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: The spectral evolution of the four SNe Icn (a) before maximum light, (b) up to 10 days after maximum, and (c) roughly 3 weeks after maximum. All wavelengths have been shifted to the rest frame, and fluxes have been normalized and shifted for display. Prominent absorption and emission features of ionized C have been marked by vertical dashed lines. (d) The Keck LRIS spectrum of SN 2019jc at maximum light in the region blueward of 5300 Å. A number of narrow absorption and emission features have been identified.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: The 56Ni mass vs. the ejecta mass of the SNe Icn (orange) fit with a CSI model, assuming a shell-like CSM structure. For comparison we plot ejecta and radioactive mass values from a sample of SESNe (Taddia et al. 2018, 2019; blue and purple) and USSNe from the literature (Drout et al. 2013; De et al. 2018; Yao et al. 2020; green). The SN Icn 56Ni masses are upper limits derived from late-time photometry; even so, they are at odds with estimates of the SESNe but are in agreement with some USSNe.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: Left: the early-time profiles of the C III λ4650 line. Spectra smoothed with a Savitzky−Golay filter are shown by the lightly shaded curves. The rest velocity is indicated by the dashed black line, while the nearby He II λ4686 line is marked by the dashed gray line. Estimated maximum wind velocities are indicated by the tick marks to the left of each absorption feature. For SN 2019hgp, two potential maxima are identified. Phases relative to g-band peak are given to the right of each spectrum. Right: same as the left panel, but for the C II λ6580 line around maximum light. The spectrum of SN 2021ckj and the earlier spectrum of SN 2019hgp were obtained from WiseRep (Yaron & Gal-Yam 2012).
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: Model CSI and 56Ni decay light curves compared to the bolometric light curves of (a) SN 2019jc, (b) SN 2019hgp, and (c) SN 2021csp. The CSI components are shown with a solid line, and the radioactive decay components are shown with a dashed−dotted line. Different fits assuming a shell-like and wind-like CSM are shown in red and blue, respectively. We find few differences between the different CSM structures. The 56Ni decay component is estimated assuming that the latest photometric epoch for each object is powered solely by radioactive decay. Our early-time observations of each object are compatible with only a CSI component, with conservative upper limits on the 56Ni mass from late-time photometry (M Ni  ≤ 0.04 M ⊙).
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: The g-band peak absolute magnitude vs. time above half the peak luminosity of the SNe Icn compared with the fast transient gold samples from Drout et al. (2014; gray squares) and Ho et al. (2021; other symbols). The SNe Icn, as well as the ultra-stripped Type Ib SN 2019dge (Yao et al. 2020), are labeled. SN 2019hgp, SN 2021ckj, and SN 2021csp occupy similar regions of parameter space to rapidly evolving SNe Ibn, but SN 2019jc is remarkably fainter and faster evolving.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption:  g–r colors of the four SNe Icn compared to those of SNe Ibn (Pellegrino et al. 2022) and a sample of ordinary SNe Ibc (Taddia et al. 2015). The colors of the SNe Icn except for SN 2019jc have been K-corrected owing to their high redshifts.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: A comparison of the estimated blackbody temperatures (top) and radii (bottom) of the SNe Icn, a sample of SNe Ibn (Pellegrino et al. 2022), and the fast transient AT 2018cow (Perley et al. 2019). The radius and temperature evolutions of the SNe Icn follow those of the SNe Ibn but are different from those of AT 2018cow.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: Extinction-corrected g-band (top) and r-band (bottom) absolute magnitudes of the four SNe Icn. Time is given relative to g-band maximum light. We also include the R-band SN Ibn light-curve template from Hosseinzadeh et al. (2017; shaded green region). Solid lines show weighted-average magnitudes at each epoch. The SNe Icn display a range of peak luminosities, rise times, and decline rates.