adsabs/AstroCLIMB huggingface dataset:
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Slow-mode solitons in the asymmetric model, for different M. (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (slow mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of the Mach number. We have taken U = 1.5, κ  e  = 3, δ 1 = 2/3, and δ 2 = 1/3 in this plot. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Fast-mode solitons in the symmetric model, for different κ  e . (a) Pseudopotential curve profile S(ϕ) vs. the electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (fast mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of κ  e . We have taken U = 1.5, M = 2.3 and δ = 0.5. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Slow-mode solitons in the symmetric model, for different M. (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (slow mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of the Mach number. We have taken U = 1.5, κ  e  = 3 and δ = 0.5. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Fast-mode solitons in the symmetric model, for different M. (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (fast mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of the Mach number. We have taken U = 1.5, κ  e  = 3 and δ = 0.5. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Velocity evolution of several lines seen in SN 2022crv. In panels 2–4, they are compared with the SNe IIb (blue color) and SNe Ib samples (red color). The error in the line velocity measurements can be as large as 500 km s−1, but this is comparable with the symbol sizes used here. The velocities are estimated using the absorption minima of the P-Cygni profiles for SN 2022crv. The velocities for the comparison sample are adopted from references in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption:  V-band absolute magnitude light curve of SN 2022crv. For the comparison SNe IIb and Ib, the magnitude scale is normalized to the peak magnitude of SN 2022crv. The values of the reference sample are taken from the papers cited in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption:  SYNAPPS modeling of the early (−9.7 days) up to a few weeks post-maximum (+23.2 days) spectra of SN 2022crv (shown in black), marked with the lines identified from the spectral modeling. The 6200 Å dip is reproduced by a combination of Hα and Si II, which we can see in the inset showing the spectra at −15.3 and −9.7 days.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Pre-maximum spectrum of SN 2022crv as compared with other members of the SNe IIb and Ib classes. The pink shaded region (top) shows the SN Ib comparison sample, the blue shaded region (middle) shows the eSN IIb, and the green shaded region (bottom) shows the cSNe IIb comparison sample. The labels include the SN name plus the date since maximum light. The data for the comparison sample are taken from WiseRep and the papers given in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Complete spectral evolution of SN 2022crv beginning at −15.3 days, up to +33.3 days. The earliest spectrum shows a prominent Hα dip which slowly diminishes around the maximum, and prominent lines of He I start developing. (The data used to create this figure are available.)
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: EW evolution of the Hα+Si II (upper) and the He I 5876 Å (lower) lines. For the comparison sample, the EWs of Hα and He I are calculated for those SNe referenced in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Apparent magnitude light curves of SN 2022crv in the BgVRIJHK filters. The g band is adapted from Seimei-TriCCS and ASAS-SN.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Post-maximum spectrum of SN 2022crv as compared with a group of SE-SNe. The layout and the comparison samples follow the descriptions in Figure 2.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Late-time spectrum of SN 2022crv as compared with a group of SE-SNe. The layout and the comparison samples follow the descriptions in Figure 2.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Electron vortexes detected by MMS during the crossing of the CS. (a) The magnitude of the magnetic field; (b) three components of the magnetic field in LMN coordinates; (c) electron density; (d) parallel temperature (black) and perpendicular temperature (blue) of electrons; (e) three components of the electron velocity in LMN coordinates; (f) energy dissipation J ·  E                   ﹩^{\prime} ;﹩ (g) magnitude of vorticity ∣∇ × V  e ∣. Four vertical gray dashed lines mark two electron vortexes, and the black horizontal dashed line in panel (g) shows the threshold (〈x〉 + 3δ) of ∣∇ × V  e ∣ for selecting the electron vortexes. The color bars at the top of the figure mark the border region (blue) and center region (red) of the CS crossing, respectively.
Paper: Beyond the Drake Equation: A Time-dependent Inventory of Habitable Planets and Life-bearing Worlds in the Solar Neighborhood
Authors: Piero Madau
Figure caption: ZAMS HZ limits for a 1 M ⊕ planet around m = 1 G-type host stars of different metallicities. The inner HZ (blue curve) is defined by the runaway greenhouse limit, while the red curve marks the outer HZ—the maximum greenhouse limit. Stellar effective temperatures and luminosities were computed following Tout et al. (1996), and the y-axis covers the range from (L ZAMS/L ⊙, T eff) = (0.70, 5635 K) at Z = 1.6 Z ⊙ to (L ZAMS/L ⊙, T eff) = (1.34, 6464 K) at Z = 0.1 Z ⊙. The effective incident fluxes determining the inner and outer HZ limits were estimated using the parametric formulae of Kopparapu et al. (2014).
Paper: Beyond the Drake Equation: A Time-dependent Inventory of Habitable Planets and Life-bearing Worlds in the Solar Neighborhood
Authors: Piero Madau
Figure caption: Abiogenesis in the solar neighborhood. Long-dashed green curve: formation rate, ﹩{\dot{N}}_{{\ell }}﹩, of life-bearing exoplanets as a function of age t 0 − t. The calculation (Equation (20)) assumes a rapid abiogenesis process with rate parameter λ  ℓ  = 1 Gyr−1, and simple life eventually arising in all TTPs, P(ℓ∣HZ) = 1. Dotted–dashed green curve: cumulative number counts of life-hosting exoplanets, N  ℓ , resulting from the integration of Equation (19). Blue curves: same for life-hosting planets undergoing a “Neoproterozoic oxygenation event” (NOE) with rate parameter ﹩{\lambda }_{O}^{-1}\,=\,3.9\,﹩ Gyr.
Paper: Beyond the Drake Equation: A Time-dependent Inventory of Habitable Planets and Life-bearing Worlds in the Solar Neighborhood
Authors: Piero Madau
Figure caption: Time-dependent HZ boundaries around GK dwarf stars. Top panel: evolution of the inner boundary of the HZ, d  i  (in au), from the ZAMS (corresponding to τ = 0) to the end of the main sequence, as a function of τ = t/t MS for stars of different mass and metallicities. Solid lines: m = 0.7 (blue), m = 0.9 (orange), and m = 1.1 (green), all calculated at Z = 0.1 Z ⊙. Dashed lines: same for Z = Z ⊙. The point on each curve denotes the time when a hypothetical planet, formed in the center of the HZ at the ZAMS stage, becomes uninhabitable. Bottom panel: HZ lifetime t HZ (in Gyr) as a function of stellar mass and metallicity. Solid blue line: Z = 0.1 Z ⊙. Dashed red line: Z = Z ⊙. The dotted lines show the corresponding main-sequence timescale.
Paper: Beyond the Drake Equation: A Time-dependent Inventory of Habitable Planets and Life-bearing Worlds in the Solar Neighborhood
Authors: Piero Madau
Figure caption: Exoplanet formation history in the solar neighborhood. Top panel: K-class dwarf (solid curve), giant planet (dashed curve), and TTP (dotted–dashed curve) formation rates in a “solar vicinity” sphere of 100 pc radius, as a function of age t 0 − t. These estimates assume η GP = 0.16 and η ⊕ = 0.24 (see text for details). Bottom panel: cumulative number counts resulting from the integration of Equation (16). Note how the solar system is younger than 77% of all TTPs, and has an age that is comparable to that of the median giant planet.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Best-fit SED (gray) from Cloudy modeling. Coplotted is the 68% C.I. range of the model predicted filter magnitude (open boxes) and the observed magnitude (circles with errorbars). Two of the bluest filters F390W and F410M (open circles and green boxes) are not used in the fit since the flux might have been significantly affected by Lyα line formation and damping wing scattering by an intervening H I column. The fitted models predict fluxes higher than observed in these two filters. The narrowband F164N filter is also not used due to potential flux calibration issues. The observed magnitudes of the extended and central component from image (10) are shown demagnified by the median predicted magnification ratio for each component applied (pink and orange circles with errors bars), as well as 68% C.I. range of the model predicted filter magnitudes demagnified in the same way (blue boxes). Best-fit central (magenta) and extended (green) component continuum contributions are separately shown.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Posterior distributions for the gas-phase abundances of C, N, Ne, and Si (arbitrary units for the vertical axis). We plot the absolute abundance on the bottom axis, and abundance relative to solar on the top axis. In the upper right panel, we observe high elevation of N abundance in the high-pressure clouds (purple) compared to the median ISM abundance at our inferred metallicity Z ≈ 0.2–0.3 Z ⊙, which indicates enrichment by massive star ejecta. By contrast, the low-pressure, more distant clouds (green) cannot be as much enriched and are consistent with uncontaminated. We also observe significant Si depletion, which is evidence for grain formation. C and Ne appear to have normal abundances. The results are also shown in Table 5.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Nitrogen abundances of the LyC cluster compared to post-turnoff dwarf stars of local globular clusters (NGC 6752 Carretta et al. 2005), star-forming regions of NGC 5253 (López-Sánchez 2007), local star-forming galaxies (Berg et al. 2022; Stephenson et al. 2023) CLASSY, and local H II regions in SDSS galaxies (Pilyugin et al. 2012). Our photoionization calculation infers a nitrogen abundance comparable to highest seen in local H II and star-forming galaxies. Our measured abundance pattern falls on a diagonal line (which goes from upper left to lower right) that is traced by abundances measured from chemically anomalous dwarf stars in the Milky Way globular cluster NGC 6752, which indicates the various degree of mixing between N-enriched gas and chemically normal gas. Finally, we also compare to GN-z11, a z ∼ 11 galaxy hosting candidate globular cluster progenitors (Bunker et al. 2023; Cameron et al. 2023; Charbonnel et al. 2023; Senchyna et al. 2023).
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Posterior distributions for the measured geometric parameters of the two clouds, including covering factors, obscuring factors, and viewing angles. Contours levels and histogram confidence intervals follow Figure 5. Refer to the two-comp. model in Table 6 for the 68% C.I.'s of the parameters.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Spatially resolved modeling of image (10). In the top panels, continuum image in F814W shows that stars in the LyC cluster can be modeled as the sum of a central unresolved component and an extended component modeled as a 1D Gaussian profile (due to lensing shear). The 1D Gaussian is centered at an angular separation 0.″015 ± 0.″001 away from the central component, with a Gaussian width σ = 0.″15 ± 0.″01. However, in the F275W filter, which probes escaping LyC radiation, the extended component is not visible. This implies that only LyC photons emitted from the central compact stellar component manage to escape.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Top: 68% C.I. for model predicted line fluxes (blue boxes) and observed line flux measured from MUSE/X-shooter (circles with errorbars). The 68% C.I. contributions from the high-pressure (purple boxes) and low-pressure (green boxes) clouds are shown separately. Bottom: 68% C.I. for model predicted line ratios (blue rectangles) and observed line ratios measured from MUSE/X-shooter (red markers).
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Posterior distributions for the measured physical parameters of the two cloud populations. Contours levels and histogram confidence intervals follow Figure 5. Parameter 68% C.I.'s are tabulated in Table 6.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Posterior distributions for star cluster parameters. 1D histograms representing the posterior distributions are marked with the mean and 68% confidence intervals (C.I.'s, dashed lines). 2D contours show the 50% and 90% levels for the density of points from PyMultinest fitting. Refer to the two-comp. model in Table 6 for the 68% C.I.'s of the parameters.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Posterior distributions for the measured ionizing photon rate, ionizing flux, and the typical distance from the cluster center for each cloud population. Contours levels and histogram confidence intervals follow Figure 5. Refer to the two-comp. model in Table 6 for the 68% C.I.'s of the parameters.
Paper: A Comprehensive Optical Search for Pre-explosion Outbursts from the Quiescent Progenitor of SN 2023ixf
Authors: Yize Dong, 一泽 董, David J. Sand, Stefano Valenti, K. Azalee Bostroem, Jennifer E. Andrews, Griffin Hosseinzadeh, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Manisha Shrestha, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: A zoomed-in section of Figure 1 close to the explosion. The precursor light curves of SN 2020tlf (Type IIP; Jacobson-Galán et al. 2022), SN 2009ip (Type IIn; Mauerhan et al. 2013), and SN 2016bdu (Type IIn; Pastorello et al. 2018) are overplotted for comparison. Toy models with a duration of 50 days and luminosities of M  r  = −9 mag and −11 mag are also shown.
Paper: A Comprehensive Optical Search for Pre-explosion Outbursts from the Quiescent Progenitor of SN 2023ixf
Authors: Yize Dong, 一泽 董, David J. Sand, Stefano Valenti, K. Azalee Bostroem, Jennifer E. Andrews, Griffin Hosseinzadeh, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Manisha Shrestha, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Limits on the pre-explosion activity of SN 2023ixf. The Clear filter is calibrated to the r band. A few precursor models from Tsuna et al. (2023) are plotted here for reference. The phases of the models are arbitrarily chosen. The typical brightness of precursor emission in SNe IIn is shown in the blue area. The brightness of precursor emission seen prior to SN 2020tlf is indicated by the purple area. The limits of our data set are generally deeper than the precursor outbursts observed in Type IIn SNe and in the normal Type IIP SN 2020tlf.
Paper: A Comprehensive Optical Search for Pre-explosion Outbursts from the Quiescent Progenitor of SN 2023ixf
Authors: Yize Dong, 一泽 董, David J. Sand, Stefano Valenti, K. Azalee Bostroem, Jennifer E. Andrews, Griffin Hosseinzadeh, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Manisha Shrestha, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Upper: the detection rate of toy-model precursor outbursts given our data set as a function of the r-band absolute magnitude for various outburst durations. The solid line only uses the r-band data. The dashed line assumes that the precursor outburst has a blackbody spectrum with a temperature of 4000 K and uses the data from all the filters. Bottom: the detection rate of a precursor outburst as a function of duration for various outburst absolute magnitudes.