adsabs/AstroCLIMB huggingface dataset:
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Upper limits on the neutron star ellipticity ϵ at the 95% confidence level. The three different colors show results for distances of 1 kpc (upper orange curves), 100 pc (middle blue curves), and 10 pc (green bottom curves). The dashed lines use a moment of inertia of I  zz  = 3 × 1038 kg m2 instead of the canonical I  zz  = 1038 kg m2 value, used by the solid lines. In the upper shaded gray area, this search is not sensitive because the high ellipticities would generate a spin-down larger than this search can probe.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Ratio between our quadrupole moment upper limits ﹩{Q}_{22}^{95 \% }﹩ and the maximum quadrupole from the upper curve in Figure 1 of Gittins & Andersson (2021). The black line marks ﹩{Q}_{22}^{95 \% }/{Q}_{22}^{\max }=1﹩, therefore our upper limits are constraining with respect to the model of Gittins & Andersson (2021) in the region to the left of this line.
Paper: Deep Very Large Telescope Photometry of the Faint Stellar System in the Large Magellanic Cloud Periphery YMCA-1
Authors: Massimiliano Gatto, V. Ripepi, M. Bellazzini, M. Dall'ora, M. Tosi, C. Tortora, M. Cignoni, M.-R. L. Cioni, F. Cusano, G. Longo, M. Marconi, I. Musella, P. Schipani, M. Spavone
Figure caption: Left: sky image of a region of radius R = 1′ around the YMCA-1 center. The red circle indicates the area defined by ﹩2{r}_{{\rm{h}}}=0\buildrel{\,\prime}\over{.} 43﹩. Center: density map of stars’ relative positions with respect to the YMCA-1 center in a circular region of 1′ in radius. We used a Gaussian function with ﹩\sigma =0\buildrel{\,\prime}\over{.} 05﹩ to smooth the map. Black points indicate the position of the stars, while the white dashed circle marks a radius R = 0.′43, namely twice the estimated half-light radius. Right: radial density profile of YMCA-1. Each point represents the density of stars in shells having a radius of 0.′05. Errors are Poissonian. The red solid line is the best fit of a Plummer model as indicated in the text, whose parameters are indicated at the center of the figure. The horizontal blue strip region marks the N bkg ± 1σ estimated values. The vertical dashed line is at R = 0.′43, namely 2r h.
Paper: Deep Very Large Telescope Photometry of the Faint Stellar System in the Large Magellanic Cloud Periphery YMCA-1
Authors: Massimiliano Gatto, V. Ripepi, M. Bellazzini, M. Dall'ora, M. Tosi, C. Tortora, M. Cignoni, M.-R. L. Cioni, F. Cusano, G. Longo, M. Marconi, I. Musella, P. Schipani, M. Spavone
Figure caption:  M V vs. r h in which we depict the position of YMCA-1 and SMASH-1 (colored stars), some old LMC GCs (magenta squares; r h taken from Piatti & Mackey 2018 and M V taken from Mackey & Gilmore 2003), and MW GCs (empty circles; taken from the Baumgardt & Hilker 2018 catalog and from Koposov et al. 2007) in this plane. We retrieved reddening values from Harris (1996, 2010 version, with some exceptions as listed in Table 1 of Gatto et al.2021b)). Finally, we also indicate the position of some confirmed and probable dwarfs (colored circles) reported in Supplementary Table 1 in Simon (2019).
Paper: Deep Very Large Telescope Photometry of the Faint Stellar System in the Large Magellanic Cloud Periphery YMCA-1
Authors: Massimiliano Gatto, V. Ripepi, M. Bellazzini, M. Dall'ora, M. Tosi, C. Tortora, M. Cignoni, M.-R. L. Cioni, F. Cusano, G. Longo, M. Marconi, I. Musella, P. Schipani, M. Spavone
Figure caption: Left: stars whose photometry was obtained with the VLT (red points) within ﹩{r}_{{\rm{h}}}=0\buildrel{\,\prime}\over{.} 43﹩ from the YMCA-1 center. In the background, as gray points, the stars whose photometry was obtained with the VST and within 30′ from YMCA-1 center. The blue solid line represents the best isochrone found with the ASteCA Python package matching YMCA-1 stars, whose parameters are reported in the top-left corner. Right: same as the left panel, but the red points are stars of a representative local field, which is a shell having an inner radius of 1′ and an outer radius set in order to have the same area adopted in the left panel.
Paper: Deep Very Large Telescope Photometry of the Faint Stellar System in the Large Magellanic Cloud Periphery YMCA-1
Authors: Massimiliano Gatto, V. Ripepi, M. Bellazzini, M. Dall'ora, M. Tosi, C. Tortora, M. Cignoni, M.-R. L. Cioni, F. Cusano, G. Longo, M. Marconi, I. Musella, P. Schipani, M. Spavone
Figure caption: Relative position with respect to the LMC center of the SCs present in the Bica et al. (2008) catalog (black dots), old GCs (magenta points), and YMCA-1 and SMASH-1. Names of the outermost old GCs are also reported in the figure.
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: Absolute V-band magnitude as a function of time in UTC on 2022 January 8 for circular apertures of fixed linear radii projected at the distance of the comet, distinguished by color. The radii of the apertures are explicitly labeled on the plot. The reported errors are dominated by the uncertainty in the assumed phase function.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Power spectral density S n, harmonically averaged over SFTs, for the three detectors as a function of frequency. The inset shows the region around the surviving outlier of the follow-up.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Upper limits on the gravitational-wave amplitude ﹩{h}_{0}^{95 \% }﹩. The lower blue curve shows the results for this search (with the shaded area showing the 1σ confidence region), while the upper orange curve shows the S6 data results of Aasi et al. (2014), the only previous search covering this frequency range. The slight discontinuity at 400 Hz is due to the change in the search grid spacings, as shown in Table 2. The upper-limit values are available as data behind the figure.(The data used to create this figure are available.)
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: The red box shows the parameter space covered by this search, while the points show the population of known pulsars in binary systems with rotational frequencies between 150 and 250 Hz. The dashed black lines indicate points of equal template density.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption:                       ﹩\overline{2{ \mathcal F }}﹩ values for each of the 19,044 candidates followed-up with the MCMC procedure as a function of the frequency of the candidate signals. The horizontal threshold line is the threshold value at ﹩{\overline{2{ \mathcal F }}}_{\mathrm{thr}}=4.34﹩.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Significance values around the candidate at 466.93 Hz when analyzing only H1 or L1 data. The vertical dashed line marks the frequency of the outlier that survives the follow-up stage.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Distribution of ﹩\overline{2{ \mathcal F }}﹩ values (averaged over segments) from the MCMC follow-up of 4763 fake signals that survive the initial stage of our search.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Significance of the top 5 × 105 candidates in each 0.1 Hz frequency band. We show the maximum, median, and minimum values. The lower-than-average values of the significance are due to the σ from Equation (5) being an overestimate of the actual standard deviation because of the noise weight being higher in the vicinity of a noise disturbance.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: The mismatch distribution of this search at four frequencies, with the other parameters spanning the ranges given in Table 1, as explained in the text.
Paper: Precursors of the RNA World in Space: Detection of (Z)-1,2-ethenediol in the Interstellar Medium, a Key Intermediate in Sugar Formation
Authors: Víctor M. Rivilla, Laura Colzi, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Andrés Megías, Mattia Melosso, Luca Bizzocchi, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Jean-Claude Guillemin, Juan García de la Concepción, Fernando Rico-Villas, Shaoshan Zeng, Sergio Martín, Miguel A. Requena-Torres, Francesca Tonolo, Silvia Alessandrini, Luca Dore, Vincenzo Barone, Cristina Puzzarini
Figure caption: Possible formation routes of 1,2-ethenediol (green box) and proposed chemical pathways for the formation of glyceraldehyde (orange box).
Paper: Precursors of the RNA World in Space: Detection of (Z)-1,2-ethenediol in the Interstellar Medium, a Key Intermediate in Sugar Formation
Authors: Víctor M. Rivilla, Laura Colzi, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Andrés Megías, Mattia Melosso, Luca Bizzocchi, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Jean-Claude Guillemin, Juan García de la Concepción, Fernando Rico-Villas, Shaoshan Zeng, Sergio Martín, Miguel A. Requena-Torres, Francesca Tonolo, Silvia Alessandrini, Luca Dore, Vincenzo Barone, Cristina Puzzarini
Figure caption: Selected unblended transitions of HOCH2CHO identified toward the G+0.693−0.027 molecular cloud and employed to perform the LTE fit. The corresponding spectroscopic information is provided in Table B1. The best LTE fit derived with MADCUBA is shown with a red curve, while the blue curve depicts the total emission considering all the species identified toward this molecular cloud.
Paper: Precursors of the RNA World in Space: Detection of (Z)-1,2-ethenediol in the Interstellar Medium, a Key Intermediate in Sugar Formation
Authors: Víctor M. Rivilla, Laura Colzi, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Andrés Megías, Mattia Melosso, Luca Bizzocchi, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Jean-Claude Guillemin, Juan García de la Concepción, Fernando Rico-Villas, Shaoshan Zeng, Sergio Martín, Miguel A. Requena-Torres, Francesca Tonolo, Silvia Alessandrini, Luca Dore, Vincenzo Barone, Cristina Puzzarini
Figure caption: Rotational diagram of (Z)-1,2-ethenediol. The red dots correspond to the transitions listed in Table 1. The black line is the best linear fit to the data points. The derived values for the molecular column density (N) and the excitation temperature (T ex), along with their uncertainties, are indicated in blue in the upper-right corner.
Paper: On the Phase-mixed Eccentricity and Inclination Distributions of Wide Binaries in the Galaxy
Authors: Chris Hamilton
Figure caption: The shape of the allowed (ω, j, j  z ) phase-space “wedge” at a fixed (arbitrary) value of Ω, showing j  z  > 0 only. Colors represent values of the initial DF, ﹩{\mathrm{log}}_{10}{f}_{0}({\boldsymbol{w}})﹩. In this case f 0 is isotropic with Gaussian eccentricity distribution, ﹩{P}_{0}{(e)=(2\pi {\sigma }_{e}^{2})}^{-1/2}\exp [-{(e-{\mu }_{e})}^{2}/2{\sigma }_{e}^{2}]﹩ where μ  e  = 0.5 and σ  e  = 0.1. Black contours on the front face of the wedge are of constant Hamiltonian H Γ, in this case for Γ = 1/3. Within each constant j  z  “slice,” the Hamiltonian flow induced by the Galactic tide transports binaries periodically around the black contours in the (ω, j) plane, leading to phase mixing—see Figure 2.
Paper: On the Phase-mixed Eccentricity and Inclination Distributions of Wide Binaries in the Galaxy
Authors: Chris Hamilton
Figure caption: Numerically computed 1D phase-mixed eccentricity DF P ∞(e) and inclination DF ﹩{N}_{\infty }(\cos i)﹩ are shown in black for different initial DFs shown in red. The P ∞ curves in the left panels are well fit by power laws P = (1 + α)e  α , shown with green dotted–dashed lines; for comparison we also show the thermal eccentricity distribution P thermal = 2e with a dashed gray line. In the right panels we show a special value of inclination, ﹩\cos i=\pm | \cos {i}_{c}| =\pm 0.894﹩, with vertical blue dotted lines—see Section 4 for details.
Paper: On the Phase-mixed Eccentricity and Inclination Distributions of Wide Binaries in the Galaxy
Authors: Chris Hamilton
Figure caption: Illustration of phase mixing. Colors show ﹩{\mathrm{log}}_{10}{f}_{0}﹩ (left) and ﹩{\mathrm{log}}_{10}{f}_{\infty }﹩ (right) in the (ω, j) phase space at fixed Γ = 1/3 and j  z  = 0.1, for the same initial DF used in Figure 1. Solid black lines show contours of constant Hamiltonian H Γ. The black dashed line shows the lowest possible angular momentum j = ∣j  z ∣.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: The evolution of the jet in negative filtergrams of SMART Hα (left panels) and in images of AIA 304 Å (middle panels) and EUVI-A 304 Å (right panels). Two small filaments and their junction are pointed out by white and blue arrows, respectively. The cyan arrows indicate the jet, and green arrows indicate the newly formed long filament. The dotted line (S0) starting at a triangle is used to derive the jet speed that is shown in the time–distance plot of panel (h1).
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: Positions of SDO (Earth) and STEREOs (A and B) for two events (https://stereo-ssc.nascom.nasa.gov/cgi-bin/make_where_gif).
Paper: A BL Lacertae Object at a Cosmic Age of 800 Myr
Authors: Ekaterina Koptelova, Chorng-Yuan Hwang
Figure caption: (a) Gemini-N/GNIRS spectrum of J2331+11 (black line). The left panel shows the enlarged view of the spectrum around the continuum break at ∼0.921 μm. The 1σ error spectrum and power law f  ν  ∝ ν −1.43 are shown with gray and dashed blue lines. The gaps in the spectrum correspond to the regions of strong atmospheric absorption. The Z-, Y-, J-, H-, and K-band fluxes measured in 2020 (quasi-simultaneously with the GNIRS spectrum) and 2021 are shown with blue and orange symbols. The red symbols show the archival fluxes in the PS1 y PS1 band (open square), UKIDSS LAS Y and J (filled circles), and H and K bands (open circles). The vertical dashed lines mark the expected wavelengths of the prominent broad emission lines of quasars. The redshift-corrected SDSS spectrum of the BL Lac J1219+36 at z = 3.59 (Paliya et al. 2020b) is overplotted in green for comparison. (b) Radio continuum of J2331+11. The flux measurements obtained with different instruments and at different epochs are shown with different symbols. The solid and dashed lines correspond to power laws f  ν  ∝ ν −0.01 and f  ν  ∝ ν −0.00 fitted to the quasi-simultaneous RACS and VLASS2.1 measurements and all multiepoch flux measurements, respectively.
Paper: A BL Lacertae Object at a Cosmic Age of 800 Myr
Authors: Ekaterina Koptelova, Chorng-Yuan Hwang
Figure caption: The SED of J2331+11. The k-corrected SED of J2331+11 (blue symbols) is shown in comparison with the k-corrected SED of the BL Lac J1219+36 at z = 3.59 (Paliya et al. 2020b; gray circles). The Z-, W3-, and W4-band flux upper limits are indicated with arrows. The black line shows the synchrotron continuum calculated using the SSC emission model.
Paper: Anisotropy of Magnetic Field Spectra at Kinetic Scales of Solar Wind Turbulence as Revealed by the Parker Solar Probe in the Inner Heliosphere
Authors: S. Y. Huang, S. B. Xu, J. Zhang, F. Sahraoui, N. Andrés, J. S. He, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, Q. Y. Xiong, Z. Wang, L. Yu, R. T. Lin
Figure caption: (a) and (b) Joint distributions obtained using the two methods of normalized reduced magnetic helicity σ m as a function of frequency and θ B. (c) and (d) Average power of spectral densities at kinetic scales in different angular bins. (e) and (f) Angular variations of the spectral index (black curves) and magnetic helicity σ m (red curves) at kinetic scales.
Paper: A BL Lacertae Object at a Cosmic Age of 800 Myr
Authors: Ekaterina Koptelova, Chorng-Yuan Hwang
Figure caption: Radio luminosity of blazars vs. redshift. The black and red open circles depict FSRQs and BL Lacs from the fifth edition of the ROMA-BZCAT multifrequency catalog of blazars (Massaro et al. 2015). The red filled star shows J2331+11. The high-redshift BL Lac J1219+36 at z = 3.59 (Paliya et al. 2020b) and the most distant FSRQ currently known, J0309+27 at z = 6.10 (Belladitta et al. 2020), are shown with an open star and a triangle, respectively.
Paper: Anisotropy of Magnetic Field Spectra at Kinetic Scales of Solar Wind Turbulence as Revealed by the Parker Solar Probe in the Inner Heliosphere
Authors: S. Y. Huang, S. B. Xu, J. Zhang, F. Sahraoui, N. Andrés, J. S. He, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, Q. Y. Xiong, Z. Wang, L. Yu, R. T. Lin
Figure caption: Spectral index (black curves) and magnetic helicity σ m (red curves) at kinetic scales in the slow ((a) and (b)) and fast ((c) and (d)) solar wind based on two selection methods.
Paper: Anisotropy of Magnetic Field Spectra at Kinetic Scales of Solar Wind Turbulence as Revealed by the Parker Solar Probe in the Inner Heliosphere
Authors: S. Y. Huang, S. B. Xu, J. Zhang, F. Sahraoui, N. Andrés, J. S. He, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, Q. Y. Xiong, Z. Wang, L. Yu, R. T. Lin
Figure caption: Magnetic spectra and spectral indices. Shown are the magnetic spectra at 18 angular bins based on methods 1 (panel (a)) and 2 (panel (b)), where the PSDs are shifted on the Y-axis for clarity, and spectral indices at MHD scales as a function of θ B using methods 1 (panel (c)) and 2 (panel (d)).
Paper: Magnetic Switchback Occurrence Rates in the Inner Heliosphere: Parker Solar Probe and 1 au
Authors: Francesco Pecora, William H. Matthaeus, Leonardo Primavera, Antonella Greco, Rohit Chhiber, Riddhi Bandyopadhyay, Sergio Servidio
Figure caption: Example of a PSP time interval containing an SB, as defined in Equation (1) and by Dudok de Wit et al. (2020). (Top panel) Magnetic field measurements at 10 s resolution. (Bottom panel) The SB, delimited by the two vertical dashed lines, is identified in the interval where z ≥ 0.5 and extends for ∼13 minutes.
Paper: Magnetic Switchback Occurrence Rates in the Inner Heliosphere: Parker Solar Probe and 1 au
Authors: Francesco Pecora, William H. Matthaeus, Leonardo Primavera, Antonella Greco, Rohit Chhiber, Riddhi Bandyopadhyay, Sergio Servidio
Figure caption: (Color plot) joint distribution J(R, ν) of SB counts per 106 km (ν) vs. PSP heliodistance (R), using the magnetic field at 10 s (a) and 60 s (d). Colors represent the probability distribution in log scale (black domains are regions with zero counts). The marginal probability distributions (see text) are shown in panels (b) and (c) for the 10 s and (e) and (f) for 60 s magnetic field. White stars represent the average value 〈ν〉 for each column, i.e., ﹩\langle \nu \rangle =\tfrac{\int d\nu ^{\prime} \nu ^{\prime} F(\nu ^{\prime} ,{R}^{* })}{\int d\nu ^{\prime} F(\nu ^{\prime} ,{R}^{* })}﹩.
Paper: Magnetic Switchback Occurrence Rates in the Inner Heliosphere: Parker Solar Probe and 1 au
Authors: Francesco Pecora, William H. Matthaeus, Leonardo Primavera, Antonella Greco, Rohit Chhiber, Riddhi Bandyopadhyay, Sergio Servidio
Figure caption: Average number of SBs per correlation length (estimated as ﹩{\lambda }_{C}\sim {10}^{6}\,{\rm{km}}\sqrt{R({\rm{au}})}﹩), as a function of the heliodistance.
Paper: Magnetic Switchback Occurrence Rates in the Inner Heliosphere: Parker Solar Probe and 1 au
Authors: Francesco Pecora, William H. Matthaeus, Leonardo Primavera, Antonella Greco, Rohit Chhiber, Riddhi Bandyopadhyay, Sergio Servidio
Figure caption: Distributions of (top) waiting times and (bottom) SB durations for the different tunable parameters—magnetic field time resolution and averaging window extension—used for PSP and for Wind. Dashed lines are reference slopes.
Paper: Precursors of the RNA World in Space: Detection of (Z)-1,2-ethenediol in the Interstellar Medium, a Key Intermediate in Sugar Formation
Authors: Víctor M. Rivilla, Laura Colzi, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Andrés Megías, Mattia Melosso, Luca Bizzocchi, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Jean-Claude Guillemin, Juan García de la Concepción, Fernando Rico-Villas, Shaoshan Zeng, Sergio Martín, Miguel A. Requena-Torres, Francesca Tonolo, Silvia Alessandrini, Luca Dore, Vincenzo Barone, Cristina Puzzarini
Figure caption: Selected unblended or slightly blended transitions of 1,2-ethenediol detected toward the G+0.693−0.027 molecular cloud. Note that each panel contains two 1,2-ethenediol transitions close in frequency that are not resolved (see Table 1), the individual contributions of which are shown with the yellow and salmon curves. The best LTE fit derived with MADCUBA for the 1,2-ethenediol emission is shown with a red curve. The blue curve represents the total emission considering all the species identified toward this molecular cloud.
Paper: The Candidate Progenitor Companion Star of the Type Ib/c SN 2013ge
Authors: Ori D. Fox, Schuyler D. Van Dyk, Benjamin F. Williams, Maria Drout, Emmanouil Zapartas, Nathan Smith, Dan Milisavljevic, Jennifer E. Andrews, K. Azalee Bostroem, Alexei V. Filippenko, Sebastian Gomez, Patrick L. Kelly, S. E. de Mink, Justin Pierel, Armin Rest, Stuart Ryder, Niharika Sravan, Lou Strolger, Qinan Wang, Kathryn E. Weil
Figure caption:  V-band light-curve evolution of SN 2013ge. The early-time data are from Drout et al. (2016), while the late-time photometry points were obtained by HST and listed in Table 1. Overplotted is the typical slope from the radioactive decay (Dessart et al. 2016), scaled to the observed light curve as a reference. The light curve shows signs of continued fading, which may signify some component of CSM shock interaction at these wavelengths. However, as for SN 1993J, the dominant blue component of the SED in Figure 3 is evidence for the emerging component of a hot, blue source not associated with the CSM interaction that we consider to be the putative progenitor companion. This scenario is discussed further in Section 3.2.
Paper: The Candidate Progenitor Companion Star of the Type Ib/c SN 2013ge
Authors: Ori D. Fox, Schuyler D. Van Dyk, Benjamin F. Williams, Maria Drout, Emmanouil Zapartas, Nathan Smith, Dan Milisavljevic, Jennifer E. Andrews, K. Azalee Bostroem, Alexei V. Filippenko, Sebastian Gomez, Patrick L. Kelly, S. E. de Mink, Justin Pierel, Armin Rest, Stuart Ryder, Niharika Sravan, Lou Strolger, Qinan Wang, Kathryn E. Weil
Figure caption: Late-time HST/WFC3 UVIS imaging of the position of SN 2013ge spanning 2016 through 2020 as summarized in Table 1. The F555W images offers the only constant filter throughout all three epochs and show the fading SN to the southeast of a constant, brighter source (“Source B”). We use the centroid of this fading source to obtain PSF photometry for the analysis in the paper, as described in the text.