adsabs/AstroCLIMB huggingface dataset:
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Mass accretion rate onto the inspiraling NS as a function of time during the simulation shown in Figure 3. In compact primaries, the NS is able to accrete above the limit at which neutrinos are able to provide the main cooling agent (red dashed line). In LMC X-4, the NS is able to gain about 0.14M ⊙, but remains well below the maximum NS mass until merging with the core (blue dashed line).
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Comparison between different types of median SEDs (normalized at rest-frame 3.6 μm). The red-solid and dotted curves represent all our lower-luminosity Hot DOG candidates, and those selected as reliable SED AGNs, respectively. The black-dashed curve represents DOGs that are not selected as lower-luminosity Hot DOG candidates. The orange and blue solid curves represent Hot DOGs (L. Fan et al. 2016) and obscured AGNs (G. Yang et al. 2023).
Paper: Molecular Gas Mass Measurements of an Active, Starburst Galaxy at z ≈ 2.6 Using ALMA Observations of the [C I], CO, and Dust Emission
Authors: Hao-Tse Huang, Allison W. S. Man, Federico Lelli, Carlos De Breuck, Laya Ghodsi, Zhi-Yu Zhang, Lingrui Lin, Jing Zhou, Thomas G. Bisbas, Nicole P. H. Nesvadba
Figure caption: Continuum maps of ALMA Bands 4 and 6 and moment-zero maps of four emission lines of PKS 0529-549. The top left and bottom left panels are the grayscale images of the ALMA Band 6 and Band 4 continuum, respectively. The red ellipse in the top left panel is the spectrum extraction aperture in this paper. The synthesized beams of the ALMA Band 4, 6 continuum images are shown as ellipses in the bottom left corners of the left panels. For the remaining four panels, we used the ALMA Band 6 continuum in the top left panel as the background image and overlaid the contours of the moment-zero maps of the corresponding lines (blue) and the ATCA 18.5 GHz radio continuum (orange). Note that the line cubes and moment-zero maps are produced with a uniform beam size of 0.″2 × 0.″2. For ATCA 18.5 GHz radio continuum, the contour levels are 1, 2, 4, 8, 12, 16 mJy beam−1. Due to the difference in the depths of ALMA Band 4 and Band 6 observations and the intrinsic strengths of the lines, the blue contours in the panels of emission lines do not represent the same intensity level. The contour levels are [2, 4, 6, 8, 12, 16] σ for [C I] (2–1), with σ = 37 mJy beam−1 km s−1; [2, 4, 6, 8] σ for CO (7–6), with σ = 38 mJy beam−1 km s−1; [2, 3, 4] σ for [C I] (1–0), with σ = 7̅5 mJy beam−1 km s−1; [2, 3, 4, 6] σ for CO (4–3), with σ = 55 mJy beam−1 km s−1, respectively.
Paper: Molecular Gas Mass Measurements of an Active, Starburst Galaxy at z ≈ 2.6 Using ALMA Observations of the [C I], CO, and Dust Emission
Authors: Hao-Tse Huang, Allison W. S. Man, Federico Lelli, Carlos De Breuck, Laya Ghodsi, Zhi-Yu Zhang, Lingrui Lin, Jing Zhou, Thomas G. Bisbas, Nicole P. H. Nesvadba
Figure caption: Extracted ALMA spectrum of PKS 0529-549. The top panel shows the Band 6 spectrum and the middle and bottom panels show the Band 4 spectrum. On top of the observed spectrum (shaded in gray), we overlay the best-fitted model using a black solid line. The model consists of assigning a Gaussian profile to each emission line and a 1D polynomial to the underlying continuum. The component of the continuum is plotted as a horizontal, black-dashed line and the components of emission lines are plotted in red and blue lines for [C I] and CO, respectively. The emission lines and the velocity centers of the fitted model, calculated with respect to z sys = 2.5725, are labeled at the top of each panel. An additional scale bar is provided to convert the frequency scale to the velocity scale. The channel widths are 11.72 MHz and 23.44 MHz for the Band 4 and Band 6 spectrum, respectively. While we only display one sideband of the spectrum in each panel, the fitting was performed by making use of both sidebands to maximize the number of channels for the continuum (see Section 3.2). Note that the continuum levels presented here do not properly account for the separation of different emission components and should not be used in further analysis (see Section 3.1 for the analysis of the spatially resolved continuum emission).
Paper: Molecular Gas Mass Measurements of an Active, Starburst Galaxy at z ≈ 2.6 Using ALMA Observations of the [C I], CO, and Dust Emission
Authors: Hao-Tse Huang, Allison W. S. Man, Federico Lelli, Carlos De Breuck, Laya Ghodsi, Zhi-Yu Zhang, Lingrui Lin, Jing Zhou, Thomas G. Bisbas, Nicole P. H. Nesvadba
Figure caption: Best-fit models of ALMA Band 4 (bottom row) and Band 6 (top row) continuum images using imfit from CASA. In each row, the left panel is the continuum image, the middle panel is the best-fit model, and the right panel is the residual image. The red contours have levels [−3, 3, 6, 9] σ, where σ = 10.6 μJy beam−1 and 10.1 μJy beam−1 for Band 4 and Band 6, respectively. In the middle panels (model images), the positions of the east and west radio lobes are marked with blue crosses. The positions of the radio lobes are estimated from the 2D Gaussian peaks of the Band 4 continuum fitting. The synthesized beam for each band is plotted at the bottom left corner of the left panel. The angular size of each image is 3″. Due to the irregular shape of the continuum of the host galaxy, the 2D Gaussian cannot fully capture the host galaxy emission and there are residual emissions in the center in both bands (see details in Section 3.1). This reflects the limitation of imfit and the potential blending of different components.
Paper: Molecular Gas Mass Measurements of an Active, Starburst Galaxy at z ≈ 2.6 Using ALMA Observations of the [C I], CO, and Dust Emission
Authors: Hao-Tse Huang, Allison W. S. Man, Federico Lelli, Carlos De Breuck, Laya Ghodsi, Zhi-Yu Zhang, Lingrui Lin, Jing Zhou, Thomas G. Bisbas, Nicole P. H. Nesvadba
Figure caption: Comparison of various emission line luminosities with the high-z galaxy sample compiled by F. Valentino et al. (2020). The line luminosities are presented in units of K km s−1 pc2. The classification of galaxies follows that of F. Valentino et al. (2020): MS = main sequence; SB = starburst; AGN/QSO = active galactic nucleus/quasar; SMG = submillimeter galaxy. Our target, PKS 0529-549, is indicated as an orange box with black edges in the figure. For the rightmost panel, ﹩{L}_{{\rm{C}}\,{\rm\small{I}}(2-1)}^{{\prime} }﹩ vs. ﹩{L}_{{\rm{C}}\,{\rm\small{I}}(1-0)}^{{\prime} }﹩, we added the lines that indicate the gas temperatures of 20, 40, and 60 K (from bottom to top), using the prescription given in N. Schneider et al. (2003) and assuming that [C I] emissions are optically thin and in LTE condition.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Archival image of the host galaxy WISEA J002356.88–142523.9 from PS1 in the g band (left) compared with the location of the transient as observed in subtracted g-band images with the Las Cumbres Observatory (right). The transient is located within 0.″1 (0.1 kpc) from the host’s center at (R.A., decl.) = (00:23:56.9, −14:25:24), as marked by the red crossbar.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Reconstructed amplitude modulation and phase diagram using the modulation frequency f  m1 and its harmonics. The signal’s shape details are visible, including a rapid ascent and a descent that starts slowly and then accelerates.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The phase evolution diagram over a time span of about 4 yr for the residuals of the Kepler LC data. Pixel shades, from black to white, indicate the mean flux in each (time, phase) bin from low to high. Each pixel represents 10 days in time axis and 0.05 in phase axis.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison of the results from multizone GRMHD simulations using two different prescriptions for the runtime per annulus: t MHD (black lines) in which the runtime is proportional to the local characteristic timescale of the annulus, and t MHDcap (blue lines), which is similar but capped at the Bondi timescale t  B . The panels show radial profiles of (a) density ρ (b) temperature T, and (c) feedback efficiency η. Because t MHDcap limits the runtime at radii larger than R  B , the outflowing energy from feedback piles up at the Bondi radius, creating a high-temperature low-density region around R  B . On the other hand, the simulation with t MHD allows enough time for the density dip to be smoothed out and for the temperature bump from feedback to propagate farther out to 107 r  g  ∼ 100 R  B . The positive feedback efficiency η in this run is constant over nearly 8 orders of magnitude in radius, all the way from the event horizon to around 100 R  B , whereas with the t MHDcap prescription, η is constant only up to ≈R  B . Regardless, both simulations agree on the most important results, namely, the density scales as ρ ∝ r −1 inside the Bondi radius, the accretion rate on the BH ﹩\dot{M}\approx 0.01\,{\dot{M}}_{B}﹩, and the feedback efficiency η ≈ a few percent.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Time-averaged radial profiles of (a) density ρ (b) temperature T (c) plasma-β, and (d) efficiency η, of a multizone GRMHD simulation initialized from GIZMO data, including the external gravity of the galaxy. The initial data from GIZMO are shown as thick blue lines and the Bondi analytical solution, normalized to the initial GIZMO density at r ≈ 106 r  g , is shown in thick gray lines. Because of feedback from strong magnetic fields, the density in the radius range R  B  − 100R  B  in the multizone GRMHD simulation (black solid lines) deviates noticeably from the initial density profile. Also, the feedback efficiency of a few percent (η ∼ 2%) is constant over 7 orders of magnitude in spatial scales. Both effects indicate that the feedback from the accreting BH is impacting the gas dynamics on large galactic scales. The temperature closely follows the Bondi solution and the plasma-β profile saturates to a value of order a few between r = 30−105 r  g  before decreasing toward the BH. Overall, the results for r < R  B  are similar to the simple GRMH. Bondi problem described in H. Cho et al. (2023).
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: The fractional change in B  y  after Δt = 100 t  g  relative to the initial magnetic field strength B 0, ΔB  y /B 0, is shown in the background color for the four tests. The velocity streamline is overlaid in black lines and the magnetic field lines in cyan. The upper panels show the result when the system is initialized with homogeneous ﹩{\boldsymbol{u}}=0.01c\,\hat{y}﹩ and ﹩{\boldsymbol{B}}\parallel \hat{x}﹩ and (a) the bflux0 prescription is used, or (b) bflux-const is used. Using the bflux0 prescription results in significant deviation from the initial conditions, while bflux-const produces no change. (c) The test is repeated for a general angle between the uniform ﹩{\boldsymbol{u}}﹩ and ﹩{\boldsymbol{B}}﹩ fields with bflux-const and the initial state is still maintained. (d) When the initial magnetic field is inhomogeneous, there is a small deviation from the initial state because the bflux-const method only translates the mean field. Overall, the ﹩{\boldsymbol{u}}﹩ and ﹩{\boldsymbol{B}}﹩ fields are less distorted compared to when the bflux0 prescription is used.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption:  θ grid in our proposed WKS coordinate system (solid blue line) compared with the widely used FMKS coordinate system (χ  t  = 0.87, α = 18; dashed orange line), both shown as functions of the code coordinate x  θ . The physical zones are x  θ  ∈ [0, 1] between the two vertical gray lines. The FMKS and WKS coordinate systems are almost identical in the physical zone 0 ≤ x  θ  ≤ 1 but differ in the ghost zones beyond the two poles.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison between two prescriptions for the magnetic fields at the radial Dirichlet boundaries. The bflux0 prescription sets the electric field Ω to 0 at the boundary, and the bflux-const prescription averages the electric field Ω over all boundary cells in the y-direction and replaces the individual Ω values with this average. This results in bflux0 having a zero flux of magnetic field across the boundary, ﹩{\bar{f}}^{x}=0﹩, and bflux-const having a constant mean flux of magnetic field to better handle the mean y-motion of the gas.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Converged BH accretion rate ﹩\dot{M}﹩ in units of the Bondi accretion rate ﹩{\dot{M}}_{B}﹩ from multizone GRMHD simulations with different values of the Bondi radius R  B . The accretion rate is suppressed more for larger values of R  B . The naive expectation, ﹩\dot{M}={\dot{M}}_{B}﹩, is shown as a gray horizontal line, and the fitted power law, Equation (15), is shown as a blue line.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison between simulations with varying resolutions and coordinate systems, some run with a single zone (one-zone) or others with the multizone method (four-zone). The run details are summarized in Table 2. The agreement across the various runs is excellent.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Time evolution of the θ-, φ-averaged angular velocity, Ω10, at r = 10 r  g , over the Keplerian angular velocity Ω K , for the (a) one-zone and (b) four-zone simulations. Solid and dotted lines correspond to episodes of positive and negative Ω10, respectively.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison of the converged t-, θ-, φ-averaged absolute angular velocity ﹩\langle \left|{\rm{\Omega }}\right|\rangle ﹩ over the Keplerian angular velocity Ω K  between the one-zone (black) and four-zone (cyan) simulations. The two profiles are broadly in agreement.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Grism images of SN 2019oyw and their background subtractions. Left-hand panels: G102 image on 2019 September 28 (top panel), its background model (middle panel), and subtraction image (bottom panel). Right-hand panels: G102 image on 2019 November 29 (top panel), its background template from epoch 2021 January 9, and subtraction image (bottom panel). These images are shown in inversed-color (i.e., black = bright).
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Image of SN 2019oyw superposing on the outer disk of SDSS J025810.28–085719.2. This image was taken with HST/WFC3/UVIS/F606W on 2020 February 16. SN 2019oyw was ∼10″ from the brightest pixel at the galactic center in the direction ∼112° with respect to north toward southeast.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Grism images on 2019 October 26 epoch in G102 (left-hand panel) and G141 (right-hand panel). Red markers mark corresponding wavelengths on SN 2019oyw’s traces. We note the markers 10750 and 11500 Å specifying the overlapping region between both filters. Another trace, which is visible in the bottom right-hand corner of each image, was from another nearby star. The vertical separation along y-axis of the traces is 4 pixels in both filters. For G102, the star’s trace contaminates starting at 10950 Å. For G141, SN 2019oyw’s trace is truncated at the red end due to low signal-to-noise ratio, and for this epoch we could extract meaningful information up to about 16500 Å, where the contamination is insignificant. We note also the truncation of the spectrum at the blue end on G102 due as well to low signal-to-noise ratio.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Environment of GRB 190829A/SN 2019oyw in F606W, F125W, and F140W. Images were taken in 2021 January, and are shown in inverse color, i.e., black = bright. The event was located at the center. Each red circular aperture is the size of 0.″39 in radius (i.e., 3 pixels in WFC3/IR and 9.75 pixels in WFC3/UVIS images). We observed a dust lane extending from north to south westwards from the aperture. We noted a bright clump (noticeable especially in F125W and F140W) associated with the dust lane on the western edge of the aperture.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Light curves of SN 2019oyw. From the late-time observations, data points are squares for detections and triangles for 3σ upper limits. For comparison, the plot also shows observations presented in Y. D. Hu et al. (2021) in SDSS’s i-filter (gray dots), and the expected light curve’s slope if powered by fully trapped Co56 (black dashed line). These values are uncorrected for Galactic and extragalactic extinction.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Images of SN 2019oyw from F140W filter. The source image taken on 2020 January 12 (left-hand panel) was subtracted by the template image taken on 2021 January 9 (middle panel), resulting in the subtracted image (right-hand panel) that clearly shows the transient. These images are shown in inversed-color (i.e., black = bright). Orientation is north-up and east-left. The cyan lines show the length scale of 1″ in each direction.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: An image of SN 2019oyw taken by HST/WFC3/UVIS/F814W on 2019 November 25 (left-hand panel). Its background model is shown in the middle panel, resulting in the subtraction image in the right-hand panel. These images are shown in inversed-color (i.e., black = bright). Orientation is north-up and east-left. The cyan lines show the length scale of 1″ in each direction.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Top: host-subtracted and Galactic-extinction-corrected optical and UV light curves of AT 2022upj, as observed by the Las Cumbres Observatory, ZTF, and Swift. The light curves in each filter are offset from one another for clarity. The gri points from Las Cumbres were subtracted with PS1 archival templates. The vertical black tick marks indicate when spectroscopy was simultaneously obtained. Middle: AT 2022upj X-ray (0.1–10 keV) luminosity from Swift XRT (red diamonds or downward arrows for 3σ upper limits) compared to the pseudo-bolometric luminosity, calculated from blackbody fits to the Swift UVOT and Las Cumbres + ZTF optical photometry (black pentagons). Bottom: the ratio of L XRT–L bol (green “x” marks). The observed X-ray output is less than 2% of the UV–optical pseudo-bolometric luminosity until after +300 days from the optical peak. The photometry and X-ray data shown in the top two panels are available in machine-readable format as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)