adsabs/AstroCLIMB huggingface dataset:
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: Comparison of the observed BgVoriz-band light curves of SN 2021agco with the models considering energy contribution from shock cooling and Ni56 decay. A total reddening of E(B − V) = 0.24 mag is applied to the extinction corrections of all observed light curves. Panels (a)–(g) show the observed luminosity compared with the best-fit model light curves in each band. The data are taken by NEXT (squares), TNT (circles), ATLAS (orange crosses), and HMT (hollow red triangles). The blue-dashed line and red-dashed line represent the shock-cooling component and the radioactive decay component, respectively. While the black lines represent the total luminosity. Notice that the z-band light curve is not included in the light-curve fitting, while the modeled light curves are still displayed in panel (g). Panel (h) displays the HMT clear band, TNT and NEXT r band, and ATLAS o-band photometry compared with the light curve modeled by a polynomial function (gray line).
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: The evolution of the pseudo-bolometric light curve, photospheric temperature, and blackbody radius of SN 2021agco compared with those of other known USSN candidates, including SN 2019dge, SN 2019wxt, iPTF14gqr, and the Ca-rich gap transient iPTF16hgs. The phases are relative to the r-band maximum as a reference for each transient. The bolometric light curves of SN 2019dge and SN 2019wxt are taken from Yao et al. (2020) and Shivkumar et al. (2023), respectively. For iPTF14gqr and iPTF16hgs, the adopted construction methods are the same as for SN 2021agco.
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: Upper panels: early-phase images of the SN 2021agco field observed by ATLAS and HMT. Lower panels: the residual images with host-galaxy template subtracted from the observed ones. The left two columns show the o-band images taken by ATLAS, and the right two show the HMT unfiltered images. The images in the first column represent the nondetections, while the second and third columns represent the first detection. The measured magnitude in each image is labeled on the top left in the lower panels. The nondetection limit of ATLAS on 2021 November 28.53 is >19.5 mag (5σ). The scale bar represents the scale of the corresponding distance at the host-galaxy redshift.
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: The correction for the HMT photometric data. Panel (a): the blue stars represent the temperature evolution of SN 2019dge taken from Yao et al. (2020). The black dotted line denotes a toy model to interpolate the SN 2019dge temperature evolution, which is expressed as T = a/(t − t 0) + b. The red square denotes the temperature evolution of SN 2021agco, which is derived from Section 2.4. Panel (b): the red points and orange crosses represent the SDSS r-band and ATLAS o-band data, respectively. The translucent red triangles denote the uncorrected HMT clear-band photometric data, while the connected red triangles denote the corrected ones. The black line represents a polynomial function to fit the joint data of the ATLAS-o, corrected HMT-clear, and r bands. Panels (c1)–(c3): the three panels display the atmosphere extinctions, transmission curves of filters, and CCD QE of HMT, TNT, and ATLAS, respectively. Panel (c4) shows the response curves of the combinations of the above three effects. Panels (d1)–(d3): the symbolic representation of the observed data is consistent with that of panel (b). In addition to combining SDSS r-band and ATLAS data, we combined uncorrected HMT data, corrected HMT data, and without HMT data for polynomial fitting. Panels (d1)–(d3) show the fitting results of the above three cases, respectively.
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: Upper panel: optical spectra of SN 2021agco. The spectral wavelength is corrected for the host-galaxy redshift, z = 0.010564. The flux density is plotted on a logarithmic scale and shifted for better display. Different colors indicate the spectra taken with different telescopes: XLT (blue), Copernico Telescope (red), Shane (orange), and LJT (green). The two spectra obtained with the Lick 3 m Shane telescope and the Lijiang 2.4 m telescope are smoothed using the Savitzky–Golay method with a window size of 61 and polynomial order of 2, with the original spectra shown in translucent colors. The number marked on the left of each spectrum indicates the phase relative to the r-band maximum. Lower panel: the Lower panel: the spectrum of the center of the host galaxy UGC 3358 of SN 2021agco (black lines) compared with a FIREFLY-modeled spectrum (red lines). The absorption features are marked by gray-dashed lines. The spectra shown in this figure are available for download with the online version of this article.(The data used to create this figure are available.)
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: Left: line velocity evolution of He I λ λ5876, 6678, 7065, Mg II λ7877, and Fe II λ5169 in the spectra of SN 2021agco, labeled in different colors (see legend). As inferred from the absorption at ∼6300 Å, the green dashed lines connecting different symbols represent the assumed velocities of Hα, C II λ6580, Ne I λ6450, and Si II λ6355. Right: He I λ5876 spectral line velocity of SN 2021agco compared with other Type Ib SNe. The red region indicates the rolling weighted average values for SNe Ib, which are taken from Liu et al. (2016).
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: The comparison of the light-curve decay timescale of the fast-evolving transients. The included transients are the same as those in the last panel in Figure 2.
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: The corner plots show posterior distributions for the joint model of the shock cooling and 56Ni decay.
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Top panels: star formation rate (SFR) vs. total stellar mass (M *) with galaxies (left) and AGN (right) as contours, with MIRONGs (light blue circles), CL AGN (dark blue squares), and TDEs (all triangles; Law-Smith et al. 2017 in red, Hammerstein et al. 2023 in pink, and Yao et al. 2023 in maroon). Following Law-Smith et al. (2017) and Dodd et al. (2021), the SFMS region is defined according to Peng et al. (2010) and designated by the solid blue line. Each line shown is separated by 1σ in SFR. Descending in SFR, the green valley is denoted as the region between the lower blue dashed line and the dashed orange line. The median error in SFR and M * is shown in the bottom right of the left plot. MIRONGs appear to closely follow the general AGN population, with a particular grouping in the highly star-forming region. Three of the four listed turn-on MIRONGs are contained in our CL AGN sample: J1115+0544, J0915+4814, and J1133+6701. Bottom panels: Hα equivalent width (EW) vs. Lick Hδ  A  absorption for the same populations. The rectangle created by the solid lines demarcates E+A galaxies, while the larger rectangle created by the dotted region more broadly designates quiescent Balmer-strong galaxies (French et al. 2016; Law-Smith et al. 2017). Median error is shown in the top right of the left plot. For consistency with Law-Smith et al. (2017), the maximum Hα EW is capped at 28 Å. However, thirteen MIRONGs have Hα EW emission values exceeding this limit and thus are not shown. Such elevated values indicate that a subgroup of MIRONGs is more highly SF than typical AGN. Interestingly, one TDE from Yao et al. (2023; AT2020neh) also has an Hα EW value in excess 28 Å. We caution that a direct comparison between the contours shown and the galaxies hosting various transient populations can only be made when the underlying selection mechanisms are taken into account. This is particularly relevant for TDE hosts (Section 5.3) but less important for CL AGN and MIRONG hosts (Appendix A).
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Top left: star formation rate vs. total stellar mass as seen in the top panel of Figure 1, this time with only AGN contours and MIRONG scatter points. The color bar indicates derived log dust mass from Jiang et al. (2021) in units of solar mass. Top right: histogram of log dust mass for MIRONGs lying in the SFMS (top) and green valley (bottom). Solid lines represent the median of each distribution, and dotted lines are spaced ± 1σ from the median. The two distributions are broadly consistent with one another, indicating that nuclear dust of MIRONG host galaxies does not vary with galaxy type. One outlying MIRONG (J154029.29+005437.2) has been excluded from all plots in this figure and is found in the green valley with a log dust mass of −3.71. Including this MIRONG only serves to broaden the standard deviations and leaves the median in place. Bottom: Balmer decrement vs. log dust mass for MIRONG host galaxies. The error bar in the top right represents the median error value for all MIRONG host galaxies in each parameter. Errors for Balmer decrement measurements are calculated from the error in Hα and Hβ line flux measurements multiplied by the recommended MPA-JHU uncertainty scaling factors of 2.473 (for Hα) and 1.882 (for Hβ).
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Host galaxy color (0,0 u − r) vs. total stellar mass for SDSS TDE reference samples (see Section 5.3 for a detailed explanation of sample selection) with the green valley region in this plane as defined by Yao et al. (2023). Left: galaxy contours with MIRONGs, MIRONGs near TDE hosts, and TDEs. Matching is performed using the methodology of Law-Smith et al. (2017), Dodd et al. (2021) with a 9% tolerance, yielding four MIRONG matches (≲11%). A box representing the matching size is shown in the lower right. Right: AGN contours with MIRONGs and CL AGN. We note that even with these additional, restrictive selection criteria, MIRONGs generally follow the AGN sample.
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: LF for MIRONGs for given luminosity bins, adapted from Figure 10 from Jiang et al. (2021). In addition to the X-ray TDEs from Figure 6 of Auchettl et al. (2018) and the optical TDEs from Figure 1 of van Velzen (2018), we additionally include the soft X-ray AGN sample from Auchettl et al. (2018). The red line is a single Schechter function fit to MIRONGs, and the fainter pink line represents the expected shift in the MIRONG distribution if a lower dust-covering factor of 0.3 is assumed (both from Jiang et al. 2021).
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Total stellar masses for all SDSS TDE reference samples (see Section 5.3 for a detailed explanation of sample selection), including galaxies, AGN, CL AGN, MIRONGs, and Y23 TDEs. Even after controlling for selection effects unique to TDEs compared to the other transients, TDEs favor lower-mass host galaxies.
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Host galaxy comparisons in total stellar mass (left) and redshift (right) for all galaxies, AGN, and MIRONGs in our catalog. The similarity between populations in each parameter makes possible the host galaxy comparison analysis that constitutes our methodology.
Paper: Mid-infrared Outbursts in Nearby Galaxies: Nuclear Obscuration and Connections to Hidden Tidal Disruption Events and Changing-look Active Galactic Nuclei
Authors: Sierra A. Dodd, Arya Nukala, Isabelle Connor, Katie Auchettl, K. D. French, Jamie A. P. Law-Smith, Erica Hammerstein, Enrico Ramirez-Ruiz
Figure caption: Sérsic-index-smoothed histograms for AGN, MIRONGs, and CL + HV AGN host galaxies. The area under the distributions is normalized to 1. Dashed vertical lines represent the median of each distribution. The MIRONG population generally display higher Sérsic indices than typical AGN.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: The top left panel illustrates the dynamical timescales of vertical mixing (solid) and horizontal transport (dashed) derived from GCM winds. The vertical mixing timescale using the fitting function in Tsai et al. (2023a) is shown in the black dot line. Horizontal transport dominates below 10−4 bar. The top right panel shows the temperatures (color scale) and winds (arrows) on the meridionally averaged equatorial plane (substellar point located at 0° longitude). The aspect ratio of the wind vector has been rescaled to 1:10 to exaggerate the vertical velocity component. The bottom left panel shows the zonal-mean zonal wind and the bottom right panel shows the temperatures and winds at approximately 1.3 mbar level.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: The VMR profiles of SO2, H2S, CO2, and CH4 at four different longitudinal locations: substellar point (0°), evening (79°), midnight (180°), and morning (259°). Results are compared to the vertical-mixing case where horizontal transport is excluded (dashed) and chemical equilibrium (dotted) to provide insights into the role of horizontal transport in shaping limb differences.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: The evolution of SO2 profile on the evening limb after the UV flux is switched off. The black dashed curve is the initial SO2 distribution, taken from the 1D VULCAN results in Tsai et al. (2023a) (no horizontal transport from other longitudes) corresponding to 80° longitude. The blue dotted line shows the global vertical mixing timescale given by Equation (2) of Tsai et al. (2023a). This evolution demonstrates that SO2 would be dissipated by the vertical mixing process after ≳10 days in the absence of stellar UV and horizontal transport.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: The left panel shows the synthetic transmission spectra of the evening and morning limbs of WASP-39b with a resolution of R = 300. The atmospheric structure and chemical composition are based on 2D VULCAN, incorporating temperature and wind profiles obtained from the Exo-FMS GCM. The models excluding horizontal transport are labeled 1D for comparison. The right panel shows the morning–evening averaged transmission spectra when assuming different atmospheric metallicities within 2D VULCAN.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: The equatorial mixing-ratio distribution of several species participating in the sulfur cycle, along with CO2, as a function of longitude and pressure on WASP-39b. The SO2 distribution when horizontal transport is omitted is shown in the upper right panel for comparison. The substellar point is located at 0° longitude.
Paper: Day–Night Transport-induced Chemistry and Clouds on WASP-39b: Gas-phase Composition
Authors: Shang-Min Tsai, Julianne I. Moses, Diana Powell, Elspeth K. H. Lee
Figure caption: Synthetic thermal emission spectra at different orbital phases (transit at 0 and eclipse at 0.5) with gas composition given by our 2D WASP-39b models (orange). The model without SO2 opacity is shown in blue and the model assuming chemical equilibrium is shown in gray for comparison.
Paper: Similarity between Compact Extremely Red Objects Discovered with JWST in Cosmic Dawn and Blue-excess Dust-obscured Galaxies Known in Cosmic Noon
Authors: Akatoki Noboriguchi, Akio K. Inoue, Tohru Nagao, Yoshiki Toba, Toru Misawa
Figure caption:  β UV vs. β opt diagram. The magenta, red, and purple stars represent JWST-EROs from Matthee et al. (2023), Barro et al. (2023), and Furtak et al. (2023b), respectively. The filled stars have β UV < −1.5 and β opt > −1.0, and the open stars have β UV > −1.5 or β opt < −1.0. The gray filled and open circles represent BluDOGs with spec-z and photo-z from Noboriguchi et al. (2022), respectively. The orange circle represents Type-1 QSO from the SWIRE template library (Polletta et al. 2007). The green triangle, square, and pentagon plots denote templates of star-forming galaxies with a metallicity of 0.2 Solar value and a constant SFR with durations of 10, 100, and 500 Myr, respectively (Inoue 2011). The black solid and dashed lines denote β opt = −1.0 and β UV = −1.5, respectively. The black arrow represents a reddening vector with E(B − V) = 0.3 for the Calzetti law (Calzetti et al. 2000).
Paper: Similarity between Compact Extremely Red Objects Discovered with JWST in Cosmic Dawn and Blue-excess Dust-obscured Galaxies Known in Cosmic Noon
Authors: Akatoki Noboriguchi, Akio K. Inoue, Tohru Nagao, Yoshiki Toba, Toru Misawa
Figure caption: Left panel: comparison of individual SEDs of eight EROs (red stars) at 5 < z < 8 found with JWST (Barro et al. 2023) and eight BluDOGs (gray circles) at 2 < z < 3 (Noboriguchi et al. 2022). The filled and open symbols represent objects with spec-z and photo-z, respectively. Right panel: comparison of average SEDs of JWST-EROs and BluDOGs. The red and orange stars represent the averages of JWST-EROs with z photo = 5.5 and 7.5, respectively. The gray filled circles represent the average of BluDOGs with spec-z. Both galaxy populations share the characteristic bimodal colors: blue UV and extremely red optical colors. All flux densities are normalized by that at the rest-frame 0.4 μm.
Paper: Similarity between Compact Extremely Red Objects Discovered with JWST in Cosmic Dawn and Blue-excess Dust-obscured Galaxies Known in Cosmic Noon
Authors: Akatoki Noboriguchi, Akio K. Inoue, Tohru Nagao, Yoshiki Toba, Toru Misawa
Figure caption: Dusty AGN populations in the context of gas-rich major merger scenario for AGN formation. The blue excess is observable through less-dusty channels produced by outflows. Therefore, its fraction is determined by the covering fraction of dusty media (C  f ) and the ratio of the timescales of the outflow phase (t outflow) to the dust-obscured galaxy phase (t DOG).
Paper: Similarity between Compact Extremely Red Objects Discovered with JWST in Cosmic Dawn and Blue-excess Dust-obscured Galaxies Known in Cosmic Noon
Authors: Akatoki Noboriguchi, Akio K. Inoue, Tohru Nagao, Yoshiki Toba, Toru Misawa
Figure caption: Diagram of SMBH mass vs. bolometric luminosity. The gray and magenta plots denote BluDOGs from Noboriguchi et al. (2022) and broad-line Hα emitters from Matthee et al. (2023), respectively. The blue dashed lines represent a constant Eddington ratio of λ Edd = 0.01, 0.1, 1.0, and 10.0.
Paper: Similarity between Compact Extremely Red Objects Discovered with JWST in Cosmic Dawn and Blue-excess Dust-obscured Galaxies Known in Cosmic Noon
Authors: Akatoki Noboriguchi, Akio K. Inoue, Tohru Nagao, Yoshiki Toba, Toru Misawa
Figure caption: Average spectrum of four BluDOGs (Noboriguchi et al. 2022). The blue line represents the dust-corrected average spectrum of BluDOGs (i.e., E(B − V) = 0.00), and the red line represents the composite quasar spectrum (Vanden Berk et al. 2001). The spectra are normalized by the flux density at 1750 Å. Black arrows and text denote the detected major emission lines. The average BluDOG spectra are available.(The data used to create this figure are available.)