adsabs/AstroCLIMB huggingface dataset:
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Proposed scenario for SN 2021foa, sketching the temporal evolution of the forward shock and the photospheric radius. In this scenario, SN 2021foa is embedded in a H-rich CSM composed of multiple shells. The precursor emission (event A) originated from the interaction of the SN forward shock with an unobserved, close CSM. From day −10 to +35, a second inner CSM with a characteristic velocity of ≈600 km s−1 is observed through the P Cygni profile of the Balmer lines. The He-rich ejecta, hidden at early epochs, is visible at day +15 after the photospheric radius reaches its maximum. The strong He I lines at this epoch sets up the “flip” in Figure 12. A rapid decline of the Hα velocity at day +35 marks the phase where the forward shock overran most of the inner CSM. After day +50, the velocity of the Hα line remains constant at ≈350 km s−1. We attribute this velocity to an outer CSM shell. The rebrightening of Balmer lines at late times (+66–+130 days) due to hydrogen recombination of a shocked SN ejecta–CSM (either the close, inner, or outer CSM), gives rise to the “flop” in Figure 12. The apparent blueshift of several lines at late times is either due to an asymmetric CSM or an effect of occultation by the optically thick photosphere close to the line-forming region of these lines, located at ∼2 × 1014 cm.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Flux ratio of Hα/He I λ5876 for the transitional SNe IIn/Ibn objects, the SNe Ibn 2006jc and the SNe IIn 2016jbu, 2009ip, and 2010jl. Each class is color coded in red (SNe IIn/Ibn), cyan (SNe Ibn), and blue (SNe IIn). The gray band encompasses the mean and one standard deviation of the line flux ratios of SNe 2011hw, 2020bqj, and 2021foa within +10 to +55 days. Fluxes are averaged in a 3-day bin.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Upper panel: light curves of the g and r bands. Lower panel: evolution of the total emission flux of H I and He I lines. The shaded region encompasses the epochs of the short photometric plateau at ≈+15 days.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Upper panel: the light curve of SN 2021foa (red) and the eight control light curves (blue) before event A (red). Bottom panel: FOM of the pre-SN light curve (red), eight control light curves (blue), control light curve number 4 (cyan), and the simulated Gaussians + control light curve number 4 (green) over ATLAS coverage (∼3 yr) up to event A of SN 2021foa. All these FOM curves were obtained after the convolution of the SNR of each light curve with a rolling Gaussian with a kernel size of τ  G  = 30 days. The simulated Gaussians have peak magnitudes of 21.4 mag, 20.21 mag, and 19.35 mag, respectively, and a fixed standard deviation of 15 days. The detection limit for our analysis was set up as FOMlimit = 15 (dashed line). The red-shaded area encompasses the precursor emission of SN 2021foa.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: VLT/X-shooter spectral region surrounding Hα of SN 2021foa. Upper panel: spectra at +95 and +427 days past peak. The black and red lines are located at the rest wavelength of Hα and [N II] λ λ6548, 6583, respectively. Bottom panel: the 2D spectrum at day +95 within the same spectral region.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Left panel: normalized VLT/X-shooter spectra of Hα, Hβ, and Paβ at v ≈ −1800 km s−1 (day +66). Right panel: normalized VLT/X-shooter spectra (+95) at v ≈ −1800 km s−1, comparing Hα, Hβ, and He I λ5016.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Evolution of the velocity of the absorption minima of H I (Hα, Hβ, Hγ, and Hδ), He I (λ λ4922, 5016), Ca II (λ λ8498, 8542, 8662), Fe II (λ λ5169, 5276, 5317), and O I λ8446 lines.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Evolution of the FWHM of H I lines. The broad and narrow emission and the absorption components are color coded (red, green, and magenta). The values of the FWHM are corrected for the resolution of the instrument. If the line was unresolved, an upper limit of the FWHM is estimated as the resolution of the instrument.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Upper panel: evolution of the velocity of the He I λ5876 for SNe Ib (Y.-Q. Liu et al. 2016, Liu16) and SNe Ibn and SNe IIn/Ibn (G. Hosseinzadeh et al. 2017, H17). Lower panel: same as upper panel, showing the evolution of the velocity of Hα broad (bold) and narrow absorption (light) components.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Evolution of the the most prominent continuum-subtracted H I and He I lines of SN 2021foa. Dashed, vertical lines correspond to zero velocity. Solid, vertical lines in panels (C), (E), (G), and (H) correspond to the velocities at the wavelengths of He I λ λ4922, 5048, 10830 and Na ID, respectively.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Left panel: evolution of the spectral region surrounding Ca II H&K. The P Cygni profile of the Balmer lines Hζ and Hϵ are prominent. Middle panel: evolution of the spectral region surrounding the pseudo-continuum produced by the blended Fe II lines. Right panel: evolution of the Ca II NIR + O I λ8446. All the regions in each panel are continuum subtracted.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Comparison of continuum-subtracted line profiles of Hα (red) and He I λ5876 (blue) of SNe Ibn 2006jc (upper row), transitional SNe IIn/Ibn 2011hw (middle row), and 2021foa (lower row) at ≈15 (left column) and ≈40 (right column) days past r-band maximum.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Decomposition of continuum-subtracted line profiles of He I λ5876 (left column) and Hα (right column) of SNe Ibn 2006jc (upper row), transitional SNe IIn/Ibn 2011hw (middle row) and 2021foa (lower row) at 2 weeks after r-band maximum. Solid and dashed lines represent the fits to the emission components of the line profiles, while dotted lines correspond to the fit to any absorption trough.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The radial metallicity gradient as a function of absolute vertical height Z above (and below) the plane. The gradient derived in this work is represented by the black dots, compared to a variety of other studies that use different tracers (J. Y. Cheng et al. (2012) (purple triangles), K. Hawkins (2023) (blue triangles), M. R. Hayden et al. (2014) (pink squares), and Y. Yan et al. (2019) (green squares)). Consistently, Δ[Fe/H]/ΔR starts off at its most negative in the plane and shallows out with greater distances from the disk. A vertical line is plotted at Δ[Fe/H]/ΔR = 0 to illustrate where the radial gradient is no longer negative. The points derived in this work lie generally in the middle of the other studies conducted.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The [Fe/H] abundances with respect to Galactocentric radius of our planar thin disk sample. The artifact at R ∼ 8 kpc is an observational effect of the over-representation of stars in the solar neighborhood. We fit a linear model to the colored data points (column-normalized planar thin disk sample), which is represented by the black line. The gray points are the running medians of [Fe/H] in 0.2 kpc bins. From this, we obtain a metallicity gradient of Δ[Fe/H]/ΔR ∼ –0.0678 ± 0.0004 dex kpc−1 and a y-intercept of 0.546 dex for the stars in our planar thin disk sample.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The azimuthal metallicity variations (δ[Fe/H] in the last panel of Figure 5) as compared to different determinations of the spiral arms. The black contours in the top panel represent the spiral arms as derived by E. Poggio et al. (2021) using main sequence stars in Gaia and the black-solid lines in the bottom panel are the spiral arms as determined by M. J. Reid et al. (2019) using high-mass star-forming regions.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: Left-hand panel: The full APOGEE planar thin disk sample colored by the metallicity. Middle panel: Each position of the data points colored by a model gradient of Δ[Fe/H]/ΔR = –0.0678 + 0.546 dex kpc−1. Right-hand panel: the residuals of the observed [Fe/H] abundances and the linear model abundances.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The vertical metallicity gradient as a function of Galactocentric radius. The gradient derived in this work is depicted by black dots, whereas the other colored points represent the gradient as determined by different tracers in other studies (M. R. Hayden et al. (2014) (pink squares), K. Hawkins (2023) (blue triangles), G. Nandakumar et al. (2022) (purple triangles), Y. Yan et al. (2019) (green squares)). The vertical metallicity gradient is at its most negative closest to the Galactic center and shallows out (Δ[Fe/H]/ΔZ approaches 0) as distance increases.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The face-on (top panel) and edge-on (bottom panel) distribution of our thin disk sample of 202,510 stars in which the hexagonal bins are colored by the logarithmic number of stars. The black contours in the top panel are the spiral arms of the Milky Way determined by M. J. Reid et al. (2019). The orange star in both panels represents the Sun.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The correlation between absolute metallicity excess (﹩\left|\delta [\mathrm{Fe}/{\rm{H}}]\right|﹩) on the y-axes and different dynamical properties on the x-axes. The hexagonal bins are colored by density, the pink stars represent the running medians in each panel, and the error bars show the standard error on the median ∣δ[Fe/H]∣ in each eccentricity bin. In the J  r  and eccentricity panels, we see a clear increasing trend hinting that stars with high eccentricities and high radial actions contribute to the variations with the largest magnitudes.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The data model panel for the elements we deem to behave monotonically with respect to Galactocentric radius. The contours are colored by the shared [X/Fe] colorbar to illustrate the varying intensities of the deviations from the linear radial gradient. The second panel represents the average [α/Fe] abundance, with the individual α-elements in the following panels. The elements with the most saturated contours, such as [Fe/H], showcase the most exaggerated deviation from the radial gradients. The α-elements appear to be loosely anticorrelated with [Fe/H], following predictions from the difference in timescales between events that mainly produce α-elements (Type II supernova) and events that mainly produce [Fe/H] (Type Ia supernova).
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: The running median [X/Fe] abundances in 0.2 kpc radial bins for 15 elements in our sample. The high-fidelity elements ([Fe/H], [O/Fe], and [Mg/Fe]) are featured on the top row. A number of these elements would not be best represented by a linear gradient, so we leave a majority of them out of our analysis. The elements included when searching for azimuthal variations in the linear gradient are the approximately linear elements: Fe, O, Mg, Si, S. To look at the α-element behavior more holistically, we averaged the α-element abundances in Figure 7.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: This figure shows δ[Fe/H] as a function of azimuthal angle (ϕ). For reference, ϕ/π = 1 is the line of sight from the Sun toward the Galactic center. The youngest age group, 0–2 Gyr (blue squares), displays the smallest deviations from zero in δ[Fe/H]. The intermediate-age group, 2–6 Gyr (green triangles), is the largest sample and has noticeable deviations from zero. The oldest age group, 6+ Gyr (purple circles), varies the most dramatically in δ[Fe/H] azimuthally. This depiction matches the theorized azimuthal variations, discussed further in Section 4.4.
Paper: [X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Zoe Hackshaw, Keith Hawkins, Carrie Filion, Danny Horta, Chervin F. P. Laporte, Christopher Carr, Adrian M. Price-Whelan
Figure caption: This figure is similar to the right-hand panel of Figure 5 but increasing age groups of 0–2, 3–6, and 6+ Gyr from left to right with 7297, 14,419, and 3890 stars, respectively. The color bars are constant throughout all panels, and thus the youngest age group has the least amount of contrast and represents the smallest deviations from the linear gradient. Conversely, the oldest age group has the most saturated colors due to the larger variations from the modeled linear gradient.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Top left: PS1 red, green, and blue false-color gri image of CSS 161010’s field. The gray square is a zoom-in on the field around CSS 161010. Known galaxies in the field are marked with magenta circles. Top right: false-color IMACS/Magellan V-band image of the field around CSS 161010. The transient is located close to the center of its faint host. Bottom: relationship between BH mass (M BH) and stellar mass (M ⋆) for a sample of galaxies (A. E. Reines & M. Volonteri 2015; D. D. Nguyen et al. 2018; J. E. Greene et al. 2020), NGC 4395 (lower value, M. den Brok et al. 2015; higher value, J.-H. Woo et al. 2019), and J0249–0815 (W. Zuo et al. 2024). The linear fits obtained by J. E. Greene et al. (2020) for the early-type (green), late-type (orange), and all galaxies (blue) are shown with solid lines. The extrapolations of these fits are shown with dashed lines. The estimated M ⋆ of CSS 161010’s host is indicated with a vertical black line, and the points where the fits cross it are highlighted with circles.
Paper: CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Claudia P. Gutiérrez, Seppo Mattila, Peter Lundqvist, Luc Dessart, Santiago González-Gaitán, Peter G. Jonker, Subo Dong, Deanne Coppejans, Ping Chen, Panos Charalampopoulos, Nancy Elias-Rosa, Thomas M. Reynolds, Christopher Kochanek, Morgan Fraser, Andrea Pastorello, Mariusz Gromadzki, Jack Neustadt, Stefano Benetti, Erkki Kankare, Tuomas Kangas, Rubina Kotak, Maximilian D. Stritzinger, Thomas Wevers, Bing Zhang, David Bersier, Subhash Bose, David A. H. Buckley, Raya Dastidar, Anjasha Gangopadhyay, Aleksandra Hamanowicz, Juna A. Kollmeier, Jirong Mao, Kuntal Misra, Stephen. B. Potter, Jose L. Prieto, Encarni Romero-Colmenero, Mridweeka Singh, Auni Somero, Giacomo Terreran, Petri Vaisanen, Łukasz Wyrzykowski
Figure caption: Spectral sequence of CSS 161010 from 9.4 to 57.7 days from the start of the outburst (JD = 2457669.92 ± 2.00). The phases are labeled on the right. Each spectrum has been corrected for Milky Way extinction and shifted vertically for presentation. A zoom-in around the Hα P Cygni profile in velocity space from 21 to 58 days is shown in the smaller right panel. Note the blueshift of Hα at all epochs.