adsabs/AstroCLIMB huggingface dataset:
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Left panel shows the J − K  S  color evolution of V2493 Cyg with J magnitude and time. The square represents the quiescent phase location of V2493 Cyg as obtained from the 2MASS survey on 2000 June 10. The dots represent the evolution of V2493 Cyg from phase (2) to phase (6) part of the LC. The red dots represent the evolution of V2493 Cyg during its transition to intermediate quiescent phase after the first outburst. Right panel shows the position of V2493 Cyg in the J − H/H − K  S  CC diagram during our monitoring period corresponding to the post second outburst phase. The square represents the quiescent phase locus of V2493 Cyg in the CC plane. The solid red line represents the locus of the classical T Tauri (CTT) stars (Meyer et al. 1997). The blue, green, and maroon dashed lines represent the reddening vectors (Rieke & Lebofsky 1985).
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Left panel shows the W1 absolute magnitude vs. W1–W2 color evolution of V2493 Cyg with magnitude and time. The quiescent phase locus of V2493 Cyg is depicted by the brown square. The model isomass curves for mass 0.3 M ⊙, A  V  = 0 mag, and A  V  = 20 mag, and those for mass 0.6 M ⊙ are also plotted (Liu et al. 2022). The right panel shows the spectral energy distribution of V2493 Cyg during our monitoring period.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Red giant branch color composite image of V2493 Cyg obtained by using the TIRSPEC K  s  (red), J (green), and 1.3 m DFOT V (blue) band images. The source V2493 Cyg is marked by a red circle. The cyan circle marks the extent of the reflection nebula that first appeared after the first outburst and has remained until date. The local standard stars that have been used for calibration of V2493 Cyg are marked by green circles.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Timescales of the different studies and surveys at optical and NIR wave bands with which the evolution of V2493 Cyg was monitored. Our monitoring program is denoted by the orange horizontal bar, and it includes monitoring in both optical and NIR wave bands. Semkov et al. (2010, 2021) monitored V2493 Cyg extensively in optical wave bands as shown. The NIR monitoring was primarily carried out by Miller et al. (2011) and Kóspál et al. (2016), which covered both the 2010 and 2012 outburst.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Upper panels: yields of iron and magnesium from AGN accretion disks for ﹩{E}_{\mathrm{SN}}=30\times {E}_{51}﹩ according to Figure 4. Metals increase with episodic time; however, some of them will be swallowed by SMBHs along with the accretion flows. Middle panels: iron and magnesium abundances produced in AGN accretion disks. Iron and magnesium abundances increase with episodic time. Lower panels: iron abundances relative to magnesium. [Fe/Mg] reaches a saturated state after ∼107  yr. The saturated values of [Fe/Mg] can reach ∼0.2 depending on the accretion of AMS in AGN disks.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The same parameters of the AMS as Figure 11, but SN explosion energy is taken as ﹩{E}_{\mathrm{SN}}=30\times {E}_{51}﹩ according to Figure 7 (very-high-winds: ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-8}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩).
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Global SED of AGNs with star formation with extinction, corresponding to Figure 4. We take M • = 108 M ⊙ and ﹩\dot{{\mathscr{M}}}=1﹩ for AGN disks, and ΔΩ = π/4 for reprocessing emissions from the torus.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The same parameters of the AMS as Figure 11, but ﹩{E}_{\mathrm{SN}}=30\times {E}_{51}﹩ according to Figure 7 (high-winds: ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩). Comparing with cases with ﹩{E}_{\mathrm{SN}}\sim {10}^{51}\,\mathrm{erg}\,{{\rm{s}}}^{-1}﹩, high-energy explosions eject more metals.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The same parameters of the AMS as Figure 11, but ﹩{E}_{\mathrm{SN}}=30\times {E}_{51}﹩ according to Figure 6 (mid-winds: ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-10}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩).
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Intrinsic SEDs of the star formation corresponding to Figure 4. Peak fluxes at extreme ultraviolet bands are mainly contributed by the massive stars. The injected stars with the Salpeter IMF can be neglected for the SED.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Intrinsic SEDs of the star formation corresponding to Figure 7 but ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-9}{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. The SEDs are generally redder than that without stellar winds.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Yields from SN explosion. Iron yields are sensitive to explosion energy (﹩{E}_{\mathrm{SN}}﹩). We use the numerical results for two extreme cases with ﹩{E}_{\mathrm{SN}}=(1,30)\times {10}^{51}\,\mathrm{erg}﹩ for iron productions, respectively.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The same parameters of the AMS as Figure 11 but the SN explosion energy is ﹩{E}_{\mathrm{SN}}={10}^{51}\,﹩ erg. Comparing with the previous ones, we find that the metal production is lower than that in ﹩{E}_{\mathrm{SN}}=30\times {E}_{51}\,﹩ erg.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: The sky map produced by using LVC localization data for the merger event S190425z and the HET track corresponding to the epoch of the alert. The LVC location of this alert is given by the green bands. The region accessible to the HET above decl. = −10° and below +71° is given by the dark blue band on the right. The lighter blue represents air mass less than 2.5. The location within 18° of the Sun is given by the large yellow patch. The lighter brown area is for air mass greater than 2.5 and the dark brown region on the left represents the portion of the sky below the horizon. The HET track overlapped with the large LVC sky map at the time of this alert. This figure provides a visual aid for observers and illustrates the technique by which we decided whether to trigger on a given LVC alert and to construct a prioritized list of galaxies to be searched for a new OT.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Completeness of the GLADE catalog in the B and K bands for different redshift ranges. The solid lines are luminosity histograms of GLADE galaxies within different distance shells in terms of their measured B-band and K-band luminosities. Dotted lines are our expectations for complete catalogs based on Schechter function measurements for each band. The GLADE catalog is designed to be more complete in the B band, but we use the K band since we aim to use the luminosity as an indicator of mass.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: A sample VIRUS (Gebhardt et al. 2021; Hill et al. 2021) image that would be used in our proposed search for the OT associated with a gravitational-wave event. Each IFU unit covers an area of 50″ on a side. The VIRUS array automatically produces a zeroth-moment image using the wavelength region 3500–5500 Å and an adopted aperture to make a collapsed image. The whole array is 21′ on a side. This image butts the IFUs together, preserving their relative position. Each of the 20,000 fibers is positioned to an accuracy of 0.″1. The faintest objects in the image are g ∼ 22–23. The streak in the upper right is a satellite or asteroid artifact.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Target galaxy GALEXASC J165500.03+140301.3. On the left is Pan-STARRS imaging of the field overlaid with Pan-STARRS cataloged sources (blue) and VIRUS point sources (red). On the right is the collapsed spectral image of a VIRUS shot of the same field cropped around a 25″ radius. The streaks across the IFU field correspond to CCD artifacts at the time of the observations and which affected point-source identification. These artifacts are primarily hot pixels and charge traps that have been subsequently identified and removed from the latest reductions.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption:  g-band (top) and r-band (bottom) magnitudes of three different two-component models with varying morphologies and average ejecta velocities (see Korobkin et al. 2021 for details). Despite the fact that the ejecta masses are the same, the different morphologies and velocities of the components produce different light curves. Because of the complex morphologies, the light curves can also vary with viewing angle.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Point-source magnitudes for all of our target fields. Transparent bins correspond to Pan-STARRS cataloged sources. Blue and orange are stacked and correspond, respectively, to VIRUS sources matched with Pan-STARRS or only detected by VIRUS. The point-source identification algorithm fails with the brightest targets, where saturation leads it to identify more than one source per target. For lower brightnesses, the mismatch can be explained by spurious continuum point-source identification both from Pan-STARRS and VIRUS.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Preliminary results of an adaptation of SCARLET to work on VIRUS spectral cubes. Images are on the same scale but with inherently different resolutions and displayed in pixel space. Upper left shows one of the extended sources modeled by SCARLET. Upper middle shows the source, rendered to the given PSF. Upper right shows the actual observation compressed along the spectrum. The colors have been mapped to the corresponding wavelengths of maximum intensity. In the bottom is a picture of the overall collected spectrum. The results are promising but need to be combined with a customized continuum grid-search routine to be usable.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Spectra from a set of compositions produced by a high-fidelity spherical wind-ejecta model at a variety of times for a range of angles using the wind disk model from Miller et al. (2020) at 0.05, 1, 2, and 4 days. Even though these results are focused on a single wind profile, varying the abundances produce a range of spectral fluxes, especially in the optical bands that vary by over an order of magnitude. The compositions studied in this plot are listed in Table A1.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: The rage of change (magnitudes/h) in the g and r bands for the models in Figure 9. All of the models are characterized by a sharp rise in the emission. But if we miss this initial rise, the evolution can vary dramatically depending on the model. Within the first 12 hr, some models decline, others continue to rise, but at a slower pace. All are characterized by rapid variability and, although other transients may exhibit this variability, this rapid variability is a strong indicator of a potential kilonova.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Spectra of ZTF19abvionh. The narrow [O II] λ3727 is from a galaxy at redshift ∼0.1 that is near to ZTF19abvionh on the sky, but unrelated. The figure shows all the data from VIRUS and LRS2-B overlaid with a spectrum of a WN type Wolf–Rayet star (25%) plus an O7I star (75%) at zero redshift. The WR components corresponding to [He II] λ4686 and Hα align with features in the spectra of ZTF19abvionh.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Galaxies contained within the GLADE catalog that are visible from HET.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: First row: receiver operator characteristic (ROC) curves for the network trained and tested directly on transient and host photometry (without using a GP interpolation scheme). The performance has been evaluated on light curve segments truncated at early, intermediate, and late times. The mean AUROCs are reported with 1σ uncertainties in the legend of each panel. Third row: the precision–recall (PR) curves for the same model applied to synthetic photometry. The AUPRCs with 1σ uncertainties are given in the corresponding legends. Second and fourth rows: ROC curves and PR curves for the same model after 200 epochs of retraining on observed light curve segments (see the text for details).
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Architecture for our RNN, which is composed of a single LSTM layer of 60 units. The photometry in each band (interpolated, padded, or both) is stacked with the photometric redshift, extinction, and host-galaxy photometry, which are repeated at each phase. This combined array serves as the input to our RNN, and the network returns a single classification prediction corresponding to the light curve segment processed.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Best-fit GP model for one simulated light curve in ZTF passbands (ZTF-g in green and ZTF-r in red) at three phases in its evolution from the time of trigger (bottom). The best-fit band-wise covariance matrix associated with each fit is shown at top. Because our model is parameterized by the covariance between observations in both time and wavelength, observations taken in a single band inform the model in the other.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: The training and testing data sets used in this work. Top: the composition of simulated events used in phase 1 of training the network. The total numbers of light curve segments in each sample are listed, and the numbers of unique transient events in each sample are given in parentheses. Bottom: the composition of spectroscopic events from the ZTF BTS used in the retraining stage (see the text for details).
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Photometric vs. spectroscopic redshifts for the galaxies in our simulated and observed samples. ZTF BTS host galaxies are shown as black points, and synthetic host galaxies are shown as the two-dimensional histogram in blue. The discreteness in observed spectroscopic redshifts is an artifact of the template-matching algorithm through which they were determined.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Same plot as Figure 6 for the 0.2 day GP model.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Same plot as Figure 6 for the 100 Time-step GP model.