adsabs/AstroCLIMB huggingface dataset:
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Rates for a variety of SN spectral types and models as a function of redshift. The SN II and SN Ibc rates from Population I/II stars are shown as the black dashed line and black dotted line, respectively, where the values at high redshift (z ≳ 2) are extrapolations based on the Population I/II CSFH (taken from Wang et al. 2017). The black solid line is for Population I/II SNe Ia based on the observed SN Ia rates truncated at z = 6. The blue and yellow shaded regions are for Population III stars with the CSFHs of the S19 and LB20 models, respectively. The solid and dotted lines in the hatched regions are obtained by using bottom-heavy and top-heavy IMFs, where the three dashed lines from top to bottom are for the top-heavy IMF with M up = 10, 50, and 500 M ⊙, respectively. The corresponding cosmic time is shown on the upper axis. The contributions from individual formation channels are not presented for clarity.
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Left panel: the influence of CSFHs on SN Ia rates. The Population III SN Ia rates are obtained based on the optimistic model, i.e., f b = 1 and top-heavy function of M up = 10 M ⊙. Right panel: the CSFHs for Population III stars in several studies from Trenti & Stiavelli (2009), Johnson et al. (2013), Mebane et al. (2018), Jaacks et al. (2019), Sarmento et al. (2019), Liu & Bromm (2020), Visbal et al. (2020), and Hartwig et al. (2022).
Paper: Type Ia Supernovae from First-generation Stars
Authors: Zhenwei Li, Lifan Wang, Zhanwen Han, Xuefei Chen
Figure caption: Upper panel: the expected number for JWST adopting a survey area of ﹩300\,{\mathrm{arcmin}}^{2}﹩ and survey time of 3 yr. The numbers of SNe II, SNe Ibc, and Population I/II SNe Ia with observational DTD are shown in black dashed, black dotted, and black solid lines, respectively. The Population III SNe Ia of the S19 and LB20 models are shown in blue and orange shaded regions, where the upper boundaries are for the optimistic model of a top-heavy IMF, and the lower boundaries are for the pessimistic model of a top-heavy IMF with M up = 500 M ⊙. Lower panel: similar to the upper panel but for the cumulative numbers.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Adopted photometric decomposition of the composite K  s -band surface brightness profile of NGC 4826 here plotted against major-axis radius r to emphasize that the galaxy is dominated in radius by its exponential disk. The lens component revealed in Figure 2 is the prominent “shelf” in surface brightness with outer radius ﹩\sim {45}^{{\prime\prime} }﹩. A Sérsic (1968) profile fit to this is shown by the outer dashed profile; it has index n Outer lens ≃ 0.17 (with K-band surface brightness μ  eK  = 16.75 at effective radius r  eK  = 23.″0). The inner components are, from the outside inward at 20 mag arcsec−2, the outer lens, a classical bulge with n Bulge = 3.27 (μ  eK  = 14.98;  r  eK  = 7.″4), the rest of the pseudobulge fitted with a Sérsic function with n PB(Part)  =  0.58 (μ  eK  = 15.96;  r  eK  = 11.″3), and an inner lens with n Inner lens = 0.18 (μ  eK  = 14.38;  r  eK  = 3.″1). The disk is approximately exponential (n = 1.07 with K-band surface brightness μ  eK  = 17.64 at effective radius r  eK  = 101.″1). The inner components are better seen in Figure 6, which plots surface brightness against r 1/4. The three parts of the pseudobulge (the outer lens, the rest of the pseudobulge [PB(Part)], and the inner lens) add up to have PB/T ≃ 0.13, almost the same as the classical-bulge-to-total luminosity ratio B/T ≃ 0.12 ± 0.02. The sum of the components shown by dashed curves is represented by the solid curve. The decomposition fit is made between the vertical dashes across the profile points (the inner one is at 0.″4).
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Adopted photometric decomposition plotted against ﹩{(r/\mathrm{arcsec})}^{1/4}﹩ to show components at both small and large radii. The lens component shown in Figure 2 proves to be the outer of two “shelves” in surface brightness; these lens components have almost the same, very small Sérsic index. In practice, we use their profiles as the data points that remain when the rest of the model is subtracted from the composite profile. Both sets of lens data points are chosen to have constant surface brightness inside the radial range where they are well measured by the composite profile and decomposition model (that is, we interpret these as lens components, not as rings that are dark inside). When the two lenses and the outer disk are subtracted from the composite profile, the rest of the galaxy is well fitted by two Sérsic functions, an inner one with n Bulge ≃ 3.27 that we identify as the classical bulge and an outer one with n PB(Part) = 0.58 that we consider, together with the two lens components, to be the pseudobulge. The classical and pseudo parts of the bulge are approximately equal in importance in this favored decomposition. See the Appendix and the discussion in Section 2.3 for alternative decompositions. Again, the sum of the components shown by the dashed curves is represented by the solid curve, and the fits are made between the vertical dashes across the profile points.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Composite surface photometry of NGC 4826 in K  s  and redder color bandpasses. The K  s -band zero-point is on the 2MASS photometric system (Cutri et al. 2003; Jarrett et al. 2000). Outside the radii of the dust disk, the 2MASS K  s  image was measured without absorption corrections; it provides the zero-point. Within the dust disk, the K  s  image was corrected for internal absorption as described in the text. The HST NICMOS NIC3 profiles were then shifted to this absorption-corrected profile. At large radii, 3.368 μm WISE and 3.55 μm Spitzer Space Telescope profiles were shifted to the 2MASS K  s  profile. The four panels show (bottom to top) major-axis surface brightness, ellipticity, major-axis position angle PA east of north, and (given that the scatter is too small to see in the bottom panel) departures of the individual profiles from the mean K  s  composite profile shown in the bottom panel by the solid black curve. It is important to note that the top panel shows that color gradients between K  s  and >3 μm are small. Here and elsewhere, photometric profiles are plotted against r 1/4 so that Sérsic n < 4 profiles (concave down) are easily distinguished from n > 4 profiles (concave up). We do not plot μ against ﹩\mathrm{log}r﹩, because no components have ﹩\mu \propto \mathrm{log}r﹩.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Multicolor color composite images of NGC 4826. The left image is a gri-band composite from the Sloan Digital Sky Survey via NED. The right image is a color composite made using the sum of 2MASS J, H, and K images for the blue channel, the Spitzer Space Telescope Channel 1 image at 3.55 μm for red and the average of the two for green. Both panels show the same field of view, the width of which is 11.′9; north is up and east is left. The right panel shows the Figure 1 HST Hubble Heritage field outlined in black. The dusty disk that dominates visible bandpasses is a slightly rim-brightened bright disk (a “lens”component) when seen in the infrared, where dust extinction is less important.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Multiband image of NGC 4826 from STScI’s Hubble Heritage project. HST data used to make the image come from two programs: GO-8591 and GO-9042. Colors are blue: F450W (B), cyan: F547M (Strömgren y), red: F656N (Hα), and pink: F814W (I). North is up; east is left, and the NE side of the galaxy is the nearside. The long axis of the rectangular bounding box is 137″. The prominent dust lanes, a clear view of the small bulge, and inclination angle of the disk are evident from the image. At small radii, there is a composite classical bulge plus pseudobulge (Kormendy & Kennicutt 2004; Kormendy 2013; Kormendy & Ho 2013a). Decoupling these components is necessary to interpret correlations between black hole mass and bulge properties. Parameters of two overlapping components are strongly coupled even in the absence of dust, and deriving them here required special care. A key revelation from our analysis is that the internally absorbed and very dark parts of the inner galaxy (in this figure) are actually higher in stellar density than the outer disk (Figure 2). To understand NGC 4826, we need photometry that is as absorption-corrected as possible.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Photometric model of the stellar light distribution at small spatial scales used in dynamical modeling. The NICMOS NIC3 profiles and the inner part of the K  s -band composite profile from Figure 3 are shown in red. A profile measurement of the ∼7200 Å STIS acquisition image is shown with green points, zero-pointed to K  s . The adopted perfect-resolution light profile used near the center of the galaxy is shown in black and (after PSF convolution) by the green curve. At radii larger than those shown here, the K  s -band composite profile (including ellipticities) was used to model the stellar light distribution.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Kinematic parameters measured from Hα, [N II], and [S II] emission lines in STIS longslit spectroscopy. From top to bottom, we show velocity, velocity dispersion, continuum flux, and equivalent width of Hα and [N II]. A vertical dotted line marks the likely dynamical center, which is notably offset from the location of the continuum maximum.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: LOSVDs from HST/STIS observations. Each panel shows the distribution of velocities in the major-axis spatial bin indicated by the radial coordinate from kinematic center. For the r = 0.″1 bin, we plot the LOSVDs from both sides in the same panel, with the sign of velocity flipped so that they may be directly compared. The error bars indicate the 1σ  uncertainties. Overall, the data show strong symmetry and high signal-to-noise, making these data good candidates for axisymmetric modeling. The best-fit model (black line) reproduces all of the major features.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Correlations of black hole mass (here designated M •) with (left) the K  s -band absolute magnitude and luminosity of the bulge component of the galaxy, (center) the bulge velocity dispersion, and (right) the stellar mass of the bulge component. These are the correlations from Kormendy & Ho (2013a) with the preliminary black hole mass for NGC 4826 replaced with the presently derived value and with the point plotted twice, once (dark red) for the adopted classical bulge parameters and again (dark red point surrounded by light blue) for the sum of the classical and pseudobulge. The thick horizontal error bars on the classical bulge points are for the 1σ  uncertainty in B/T quoted in Figures 5 and 6. The thin horizontal error bars end at the bulge parameters for the extreme “error bar” decompositions illustrated in the Appendix.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Maximal-pseudobulge photometric decomposition plotted against ﹩{(r/\mathrm{arcsec})}^{1/4}﹩ to show components at both small and large radii. In this fit, the parameters were derived to maximize the pseudobulge-to-total ratio PB/T while still producing an acceptable global fit. This procedure required forcing the classical bulge Sérsic index to its lowest value. The lens components are treated as they are in our adopted fit. The classical bulge component contributes roughly half as much light as the pseudobulge, but it still dominates the light inside of ﹩{(r/\mathrm{arcsec})}^{1/4}=1.5﹩. The low classical bulge to total ratio, while not ruled out, is small for an Sab galaxy. Data and symbols are the same as in Figure 6.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Minimal-pseudobulge photometric decomposition plotted against ﹩{(r/\mathrm{arcsec})}^{1/4}﹩ to show components at both small and large radii. Here, the lens components are treated as they are in our adopted fit, and together they are assumed to be all of the pseudobulge. Thus the rest of the profile is decomposed into two Sérsic components to represent a classical bulge and disk. The statistical uncertainties in this fit are small. However, the classical bulge has n = 4.28, larger than values normally seen in small bulges, and the disk Sérsic index n = 0.87 ± 0.04 < 1 is smaller than n = 1 for an exponential. Data and symbols are the same as in Figure 6.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Modeling results. Each panel plots χ 2 against one of the model parameters (clockwise from top left: black hole mass, mass-to-light ratio, dark matter halo core radius, and dark matter halo asymptotic velocity). Each model is plotted with a black circle, and the best-fit model is plotted with a larger red circle. The purple curves are smoothed traces of the minimum χ 2 at each parameter value and show the marginalized χ 2 curve. From bottom to top, the horizontal lines show the minimum χ 2, ﹩{\chi }_{\min }^{2}+1﹩, ﹩{\chi }_{\min }^{2}+4﹩, ﹩{\chi }_{\min }^{2}+9﹩ to show 1, 2, and 3σ  regions for one interesting parameter. The χ 2 curves are unimodal and roughly parabolic near the minimum, indicating robust results. The best-fit mass with 1σ  uncertainty is ﹩M={8.4}_{-0.6}^{+1.7}\times {10}^{6}\ {{\rm{M}}}_{\odot }﹩ and is marginally consistent with M = 0 at about the 3σ  level.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Mass-to-light ratio radial profiles both local (solid blue curve) and enclosed (dashed orange curve). These profiles come from the 20 models with the lowest χ 2 and show the range of plausible values. The local ϒ K (R) shows a flat inner portion with a slight increase starting at R ≈ 10″. The enclosed ϒ(R) shows the black hole dominating the total mass-to-light ratio inside of R = 1″.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Orbital anisotropy of the models. We plot, as a function of radius, the ratio of radial velocity dispersion to the tangential (azimuthal and polar) velocity dispersion. The solid line is from the best-fit model, and the shaded region comes from the range of values of the 20 best-fit models to estimate the uncertainty. At large radii, the orbits are tangentially biased owing to the disk. At smaller radii, the tangential bias may indicate a depletion of radial orbits from the earlier dynamical activity that produced the counter-rotating gas streams.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Central 15″ × 15″ of NGC 4826 as observed with Chandra in the 0.2–7 keV band (left), the hard 2–7 keV band (center), and with HST/WFPC2 through the F656N filter. The full band X-ray image shows distinct point sources as well as diffuse emission. The hard band X-ray image shows a relatively small amount of emission coming from the central region, but there is a potential hard X-ray point source (location indicated by a circle in all three panels) that is consistent with the stellar surface brightness peak; though, it requires deeper X-ray imaging to fully assess.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: LOSVDs from HET observations. Each panel shows the distribution of velocities along the major (blue) and minor (orange) axes in the spatial bins indicated in each panel as distance from the kinematic center. The major-axis LOSVDs show rapid rotation in the outer parts of the galaxy, where the light is dominated by the disk, whereas the minor-axis LOSVDs are centered at V = 0, as would be expected in an axisymmetric system. The black line shows the best-fit model.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Velocity and velocity dispersion profiles from HST/STIS data and the best-fit model. Although the model is not fit in this space, it is shown to produce a good match to the profiles and demonstrates how the dispersion peak is just off of R = 0 with substantial rotation about the center.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Left: primary and secondary ETVs of the inner binary constructed from the TESS FITSH data. The three panels each cover two sectors of TESS data (as labeled in the lower left corners), i.e., about two cycles of the outer orbit. Red (blue) points represent primary (secondary) eclipses. The smooth curves are model fits from the photodynamical analysis (see Section 4). The vertical dashed and dotted–dashed lines represent the locations of TESS observed eclipses where the binary eclipses the distant tertiary and vice versa, respectively. The lower panels represent the corresponding residuals. Right: same as the left panel, but zoomed out to cover an interval of about 8 yr. The black sinusoidal curve represents the pure LTTE contribution. This nicely illustrates that on a yearly timescale the ETV is chiefly dominated by the third-body perturbation effects (including the dynamically driven apsidal motion as well, but on a bit longer timescale, the LTTE, caused primarily by the fourth component, becomes dominant).
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: From Kormendy (2020), parameter correlations for elliptical galaxies and classical bulges of disk galaxies (dark gray) and for spheroidal galaxies (light gray). The bottom panels show effective radius r  e  that contains half of the total light and effective surface brightness μ  e  at r  e  correlated with the V-band absolute magnitude of the component. The top panel shows the Kormendy (1977) relation, μ  e  vs. r  e ; this projection shows the fundamental plane nearly edge-on and has especially small scatter. Sources are given in keys, references omitted here are in Kormendy & Bender (2012). Galaxies in which supermassive black holes are detected via spatially resolved stellar or gas dynamics are encoded in dark red for ellipticals and dark brown for bulges. Our three classical bulge models for NGC 4826 are shown in green; the middle point is for the preferred decomposition.
Paper: The Black Hole Mass and Photometric Components of NGC 4826
Authors: Kayhan Gültekin, Karl Gebhardt, John Kormendy, Adi Foord, Ralf Bender, Tod R. Lauer, Jason Pinkney, Douglas O. Richstone, Scott Tremaine
Figure caption: Faber & Jackson (1976) correlations for ellipticals with and without a “core,” i.e., a break in the density profile near the center from a steep outer profile to a shallow inner cusp. Total absolute magnitudes and velocity dispersions are from Lauer et al. (2007) with classification corrections from Kormendy et al. (2009) and Kormendy & Bender (2013). Galaxies with dynamical black hole detections are labeled. The lines are symmetric least-squares fits (Tremaine et al. 2002) to the core galaxies (black line with gray 1σ  uncertainty) and the coreless galaxies (red line with pink 1σ  uncertainty). The kink at σ ≃ 250 km s−1 was also emphasized by Lauer et al. (2007). This figure is from Kormendy (2020) with the three classical bulge models for NGC 4826 added. All are consistent with the correlation for coreless ellipticals. The smaller bulges are slightly favored.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Tightness of triply eclipsing triple systems (P out/P in) as a function of the system compactness. λ Tau (marked by a blue symbol) is not triply eclipsing, but it is otherwise such a noteworthy benchmark system that we include it for reference. TIC 290061484, announced here and highlighted with a large open circle, is the most compact triple system known to date.