adsabs/AstroCLIMB huggingface dataset:
Paper: Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo
Authors: Justin S. Spilker, Christopher C. Hayward, Daniel P. Marrone, Manuel Aravena, Matthieu Béthermin, James Burgoyne, Scott C. Chapman, Thomas R. Greve, Gayathri Gururajan, Yashar D. Hezaveh, Ryley Hill, Katrina C. Litke, Christopher C. Lovell, Matthew A. Malkan, Eric J. Murphy, Desika Narayanan, Kedar A. Phadke, Cassie Reuter, Antony A. Stark, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiß
Figure caption: [C II] spectra of each identified clump (colors, labeled), the sum of the clump spectra (gray), and the total source-integrated emission (black). The clumps are kinematically (and spatially; Figure 2) distinct, and together comprise ≈70% of the total [C II] emission.
Paper: The Archival Discovery of a Strong Lyα and [C II] Emitter at z = 7.677
Authors: Francesco Valentino, Gabriel Brammer, Seiji Fujimoto, Kasper E. Heintz, John R. Weaver, Victoria Strait, Katriona M. L. Gould, Charlotte Mason, Darach Watson, Peter Laursen, Sune Toft
Figure caption: The location of Y002 in the plane of observables. Left column: M UV vs. β; M UV vs. L Lyα ; FWHM[C II] vs. M UV; SFRUV + SFRIR vs. L [C II]. Right column: EW0(Lyα) vs. Δv Lyα ; M UV vs. Δv Lyα ; L [C II] vs. Δv Lyα ; redshift vs. Δv Lyα . In each panel, the red filled star marks the location of Y002. The filled circles show the compilation of z ∼ 6–7 Lyα and [C II] emitters from Matthee et al. (2019) and Hashimoto et al. (2019) color-coded as labeled. Filled stars indicate the galaxies from the REBELS survey with Lyα detection presented in Endsley et al. (2022) (β values from Bouwens et al. 2021b). Sources from the ALPINE survey at z ∼ 4–6 are shown in gray (Béthermin et al. 2020; Cassata et al. 2020; Faisst et al. 2020). The dashed lines in the bottom-left panel mark the SFR–L [C II] relation as a function of metallicity as in Vallini et al. (2015). The ones in the M UV–Δv Lyα  panel show the median relation as a function of redshift in Mason et al. (2018a). The red symbols and lines in the bottom-right panel indicate the average values and the best-fit linear and parabolic trends as in Cassata et al. (2020).
Paper: The Archival Discovery of a Strong Lyα and [C II] Emitter at z = 7.677
Authors: Francesco Valentino, Gabriel Brammer, Seiji Fujimoto, Kasper E. Heintz, John R. Weaver, Victoria Strait, Katriona M. L. Gould, Charlotte Mason, Darach Watson, Peter Laursen, Sune Toft
Figure caption: Top: bidimensional spectrum of Y002 smoothed with a Gaussian filter for display purposes. Center: the red and gray areas show the optimally extracted spectrum around the region of Lyα emission at z = 7.677 and the associated noise, binned by a factor of 2 for clarity. The blue and black lines and shaded areas indicate the best simple and skewed Gaussian models and their confidence intervals. Bottom: the ALMA Band 6 spectrum of Y002 where the velocity zero point corresponds to the systemic redshift of z = 7.677 set by the [C II] line. The golden area marks the channels used to optimize the S/N for the extraction. The blue and red lines and shaded areas indicate the Lyα Gaussian models and their confidence interval as labeled, arbitrarily rescaled in flux density. We adopted the optical radial velocity definition.
Paper: The Archival Discovery of a Strong Lyα and [C II] Emitter at z = 7.677
Authors: Francesco Valentino, Gabriel Brammer, Seiji Fujimoto, Kasper E. Heintz, John R. Weaver, Victoria Strait, Katriona M. L. Gould, Charlotte Mason, Darach Watson, Peter Laursen, Sune Toft
Figure caption: Left: 8″ × 8″ cutouts of ALMA/[C II] and optical to near-IR images from the COSMOS2020 catalog (Weaver et al. 2022). The cutouts are color-scaled within ±3× rms in each image and are aligned N–E. The blue contours and slanted lines show the ALMA/[C II] 2σ–5σ levels and the Keck/MOSFIRE slit orientation. The size of the ALMA beam is shown in the first cutout. Right: best-fit photometric model of the SED with BAGPIPES at fixed z = 7.677 and its uncertainty (red line and shaded area). Empty and filled blue circles mark the photometry from the COSMOS2020 catalog (Weaver et al. 2022) and our custom re-extraction.
Paper: The Archival Discovery of a Strong Lyα and [C II] Emitter at z = 7.677
Authors: Francesco Valentino, Gabriel Brammer, Seiji Fujimoto, Kasper E. Heintz, John R. Weaver, Victoria Strait, Katriona M. L. Gould, Charlotte Mason, Darach Watson, Peter Laursen, Sune Toft
Figure caption: Modeling of the [C II] emission with single (top) and double (bottom) elliptical Gaussians. The cross shows the location of the rest-frame UV and optical emission. The white ellipses show the locations of the peaks of the modeled [C II] emission and their uncertainties. Blue lines in the left panels show 2σ–5σ contours. The images are color-scaled within ±3× rms.
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Main panel: In orange, the probability distribution of the aligned component of the primary BH spin a 1,z  for BBH systems, inferred under the model described in Section 4.2 in which the primary spin distribution consists of a nonspinning component and an aligned spin a 1,z  > 0 component, while the secondary spin is fixed to zero. The two components of the primary spin distribution are shown by the unfilled dashed and dotted bands, whereas the total distribution is shown by the filled bands. In blue, the inferred distribution of BH spins in observed HMXBs, assuming spins perfectly aligned with the orbits. Inset: Zoom-in of the aligned a 1,z  > 0 component of the BBH spin distribution (orange), compared to the observed HMXB spin distribution under different assumptions for the spin-tilt distribution, with ﹩{\sigma }_{\cos t}=0.2﹩ (purple, filled bands) and ﹩{\sigma }_{\cos t}=0.5﹩ (green, unfilled).
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Empirical CDF for the three observed HMXB BH masses (blue error bars), compared to the GW population inference. Purple bands show the CDF of the 44 observed BBH primary masses, before correcting for GW selection effects. Correcting for GW selection effects, the fit to the astrophysical BBH primary mass distribution is shown by the green, unfilled bands. Finally, we add in a small-sample-size Poisson uncertainty, showing the predicted CDF of three random draws from the astrophysical BBH primary mass distribution (orange bands). Here and throughout all figures, shaded regions show the 50% and 90% credible intervals. We see that while the observed BBH distribution (purple) skews to much larger masses, accounting for GW selection effects (green) and Poisson uncertainty (orange) brings the two distributions into agreement within statistical uncertainties, so that there is no evidence that BHs in the observed HMXBs follow a different mass distribution from the astrophysical BBH population.
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Inferred CDFs of the BH spin magnitude a for the three populations: BBH spin distribution (orange, fit taken from Abbott et al. 2021b in which both BH spins in a BBH are identically and independently distributed), observed HMXB spin distribution (blue), and observed LMXB spin distribution (pink). Following Abbott et al. (2021b), the spin magnitude distribution is fit to a beta distribution, with flat priors on the hyperparameters μ and σ 2, excluding singular beta distributions. The distribution of prior CDFs is shown by the unfilled black bands. The BBH spin distribution is skewed to small spins, peaking at the smallest spin magnitudes allowed by the prior, whereas the observed HMXB and LMXB spin distributions have most of their support at large spins a ≳ 0.4.
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Empirical CDF for the 20 observed LMXB BH masses (pink error bars), compared to the predicted CDF of 20 random draws from the astrophysical BBH primary mass distribution (orange bands) and the predicted CDF of 20 random draws from the BBH primary mass distribution conditioned on m 2 < 8 M ⊙ (green bands). The BHs in LMXBs are lower mass than the full BBH primary mass distribution, as seen by the offset between the pink curve and orange bands, but may be consistent with the inferred distribution of BBH primary masses with small secondary masses.
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Fraction of BBH systems with primary spins consistent with the observed HMXB spin-magnitude distribution, inferred under three different assumptions of the HMXB-like spin-tilt distribution: perfect spin–orbit alignment (blue, unfilled), small possible tilts ﹩{\sigma }_{\cos t}=0.2﹩ (purple, dashed, filled), and possibly large tilts ﹩{\sigma }_{\cos t}=0.5﹩ (green, filled). The HMXB-like fractions inferred here should be considered an upper limit; as discussed in the text, our model intentionally assigns the largest possible fraction of BBH systems to have high aligned primary spins.
Paper: Apples and Oranges: Comparing Black Holes in X-Ray Binaries and Gravitational-wave Sources
Authors: Maya Fishbach, Vicky Kalogera
Figure caption: Posterior PDF on the amount of BH spin-up in observed LMXB BHs relative to BBHs, a LMXB − a GW (pink), vs. the amount of LMXB spin-up relative to HMXBs, a LMXB − a HMXB (blue). We infer that if LMXB BHs are born with the same spin distribution as BBHs, more than 91% of observed LMXB must have been spun up with a LMXB − a GW > 0, gaining an average spin magnitude of ﹩{0.47}_{-0.11}^{+0.10}﹩. On the other hand, if the observed LMXB BHs are born with the same spin distribution as the observed HMXB BHs, only a minority of systems could have experienced spin up.
Paper: The Formation of Intermediate-mass Black Holes in Galactic Nuclei
Authors: Sanaea C. Rose, Smadar Naoz, Re'em Sari, Itai Linial
Figure caption: Similar to Figure 3, we plot the initial masses vs. initial distance (gray) and final mass vs. final distance (red) for 500 BHs. This simulation includes relaxation processes, including mass segregation, diffusion, and dynamical friction. We assume α = 1.75 for the GN density profile. Faded stars represent BHs that merge with the SMBH. As a result of inward migration, BHs merge more quickly with the SMBH, before they can become as massive as those in Figure 3. Additionally, more BHs become EMRIs and IMRIs. Additionally, in the third panel, we show a histogram of the simulated IMBH masses for two different values of α, 1.5 (orange, solid), 1.75 (red, dashed), and 2 (purple, dashed–dotted), accounting for relaxation processes. We also show the results for a simulation with α = 1.75 that accounts for momentum-driven winds (black, dotted). Despite the substantially reduced accretion, BHs in the mass gap still form.
Paper: The Formation of Intermediate-mass Black Holes in Galactic Nuclei
Authors: Sanaea C. Rose, Smadar Naoz, Re'em Sari, Itai Linial
Figure caption: We plot the relevant timescales, including collision (green), relaxation (gold), and BH–BH GW capture (purple), for a single BH in the GN as a function of distance from the SMBH. For the collision timescale, we assume the BH is on a circular orbit. The timescales depend on the density, so we adopt a range of density profiles, bounded by α = 1 (dashed curve) to α = 2 (dark, solid curve). The dark blue line represents the time for a 105 M ⊙ BH to merge with the SMBH through GW emission.
Paper: The Formation of Intermediate-mass Black Holes in Galactic Nuclei
Authors: Sanaea C. Rose, Smadar Naoz, Re'em Sari, Itai Linial
Figure caption: On the right, we plot final masses of 500 BHs using different values of α in the density profile, shallow (α = 1) to cuspy (α = 2). For the latter case, the purple line shows the analytical result from Equation (8), taking m initial to be the average mass of the population. Faded stars indicate BHs that merged with the SMBH through GWs. On the left, we plot the masses and merger times of these BHs.
Paper: The Formation of Intermediate-mass Black Holes in Galactic Nuclei
Authors: Sanaea C. Rose, Smadar Naoz, Re'em Sari, Itai Linial
Figure caption: We consider an example that highlights the mass growth as a function of distance from the SMBH. Gray dots represent the initial masses and distances from the SMBH of the BHs involved in the simulation. For simplicity, we set the initial mass equal to 10 M ⊙ for all of the BHs. Assuming the density profile of stars has α = 1, we consider two cases: BHs accrete all of the star’s mass during a collision (red) and only a portion of the star’s mass is accreted during a collision given by Equation (6) (blue). The latter case results in less growth closer to the SMBH where the velocity dispersion becomes high. The shaded regions and dashed lines represent the analytical predictions detailed in Section 2.4.
Paper: Limiting the Abundance of LIGO/Virgo Black Holes with Microlensing Observations of Quasars of Finite Size
Authors: A. Esteban-Gutiérrez, E. Mediavilla, J. Jiménez-Vicente, N. Agües-Paszkowsky, J. A. Muñoz, S. Heydenreich
Figure caption: Probability distributions of microlensing flux magnifications for a population of 20% stars with 0.2M ⊙ plus 80% smooth dark matter (orange curve) and a population of 20% stars with 0.2M ⊙ plus 80% LIGO/Virgo-type BHs of 30M ⊙ (blue curve). The left panel is for a source of 0.2 lt-days. The right panel is for a source of 10 lt-days. The scaling has been chosen to give the unit area under the PDF curves. The shaded blue area marks the region containing ∼70% of the observed microlensing magnifications (Pooley et al. 2007), i.e., with the ordinate chosen to enclose 70% of the probability (see text).
Paper: The Composition and Power of the Jet of the Broad-line Radio Galaxy 3C 120
Authors: Andrzej A. Zdziarski, Dakalo G. Phuravhathu, Marek Sikora, Markus Böttcher, and James O. Chibueze
Figure caption: A sketch of the pair-producing geometry based on Figure 2(a) of Barkov & Komissarov (2008), which shows the result of their GRMHD simulation for strongly magnetized accretion on a BH with the mass of 3M☉ and the spin parameter of a* = 0.9. The contours show the magnetic field lines, the arrows show the velocity field, and the color contours show the baryonic rest-mass density, ρ, in a logarithmic scale in ﹩{\mathrm{log}}_{10}\rho ﹩ in units of g cm−3. The jet base, shown in blue, has a very low matter density. We show e± pair production within the jet base with the arrows representing pair-producing photons and the pairs.
Paper: The Composition and Power of the Jet of the Broad-line Radio Galaxy 3C 120
Authors: Andrzej A. Zdziarski, Dakalo G. Phuravhathu, Marek Sikora, Markus Böttcher, and James O. Chibueze
Figure caption: The radio-to-IR spectrum of the core of 3C 120 from various measurements compiled in Giommi et al. (2012). The red dashed line gives a fit of the broken-power-law approximation to the partially synchrotron self-absorbed jet spectrum, Equation (A1).
Paper: The Composition and Power of the Jet of the Broad-line Radio Galaxy 3C 120
Authors: Andrzej A. Zdziarski, Dakalo G. Phuravhathu, Marek Sikora, Markus Böttcher, and James O. Chibueze
Figure caption: The blue symbols show the average 1992–1997 Compton Gamma Ray Observatory OSSE spectrum of 3C 120 from Woźniak et al. (1998). The red line gives the best power-law fit in the 50–500 keV range. For comparison, we show the 2004–2013 average spectrum (Oh et al. 2018) from the Neil Gehrels Swift BAT (fitted separately by a power law, not shown).
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: A phase-folded light curve with zooms on possible primary and secondary eclipses. The black points correspond to the actual data, while the red light curve represents a best-fit curve derived from the frequencies removed when prewhitening the orbital harmonics. The boxes in the top panel mark the locations of the zoomed-in plots, where arrows identify the start and end of potential eclipses. The best-fit light curve was smoothed with a Savitzsky–Golay filter (Savitzky & Golay 1964) to remove any short-term variability not arising from the orbital modulations. The blue, yellow, and gray curves in the top panel are reconstructions of the multiplets ν01, ν02, and ν03, with amplitudes equal to their actual values but offset vertically for clarity.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: The Fourier amplitude spectrum in the range of the pulsation frequencies, with successive plots (going row by row) that highlight the sequential prewhitening of frequency multiplets. The central components of these multiplets are indicated with their identifiers according to Table 1, and the blue arrows point at all of the multiplet components.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: Échelle diagram of the pulsation frequencies with respect to the orbital frequency. The size of the filled circles is proportional to the amplitude of that particular constituent of the multiplet. The upper panel shows the full range of frequencies; the lower panels are zooms into regions that are not resolved in the upper panel but contain multiple sequences of frequencies. These regions are denoted by rectangles in the upper panel. The x-axis label “Echelle Phase” is defined as the pulsation frequency modulo the orbital frequency, normalized to the orbital frequency. All observed modes have been labeled.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: Pulsation phase and amplitudes for multiplets centered on the frequencies ν01, ν02, ν03, and ν04; these were calculated from the analytical expressions in Equations (5) and (6). Red lines represent formal 1σ uncertainties on the values of amplitude and phase; following Montgomery & O’Donoghue (1999), these were calculated as ﹩{\sigma }_{\mathrm{ampl}}=\sqrt{2M/N}{\sigma }_{a}﹩, where the observational rms scatter per single data point σa = 14.61 mmag, N is the number of data points (190, 194), and M is the number of detectable peaks in the mode (6–8). In turn, σph = σampl/a(Φorb), where a(Φorb) is the amplitude at a given orbital phase Φorb. Blue arrows on the phase plots, denoting a length of π, provide a sense of scale. The dotted green lines in the second row of plots denote a pulsation amplitude of zero, i.e., locations where the pulsation phase cannot be meaningfully calculated.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: Comparing observed modes (circles) and modeled modes (lines) for a subset of the pulsations of TIC 68495594. The top panels compare amplitudes (normalized to maximum), while bottom panels compare mode phases, as a function of orbital phase. Columns are labeled by the ℓ and m value most likely to correspond to the observed mode. The modeled modes are selected by choosing modes with the appropriate value of m, frequencies near ∼290 day−1, and with luminosity fluctuations larger than the surrounding modes (such that the mode is not strongly trapped in the core and is not dominated by high-ℓ components). Note that phases −π and π are identical, so the match with the phases of the ν1 and ν3 modes is better than it appears.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: Pulsation amplitude and phase over two orbital cycles for the multiplet centered on ν22 (similar to Figure 4). The pulsation amplitude peaks near orbital phases 0.125, 0.375, 0.625, and 0.875 and has phase “jumps” near phases 0.25, 0.5, 0.75, and 1, corresponding to amplitude minima. These can be ascribed to modes dominated by tidally aligned ∣m∣ = 1, ℓ = 2 modes.
Paper: Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion
Authors: Rahul Jayaraman, Gerald Handler, Saul A. Rappaport, Jim Fuller, Donald W. Kurtz, Stéphane Charpinet, and George R. Ricker
Figure caption: Propagation diagram for our M = 0.5 M⊙ sdB stellar model, showing the Brunt–Väisälä frequency (N; blue line), ℓ = 1 Lamb frequency (L1; red dashed line), the lowest-order radial modes (ℓ = 0, n = 1, 2; green dotted lines), and the observed pulsation frequency range (black solid lines). The top panel is a model just before core helium depletion, while the bottom panel is just after core helium depletion; the latter is the model used in the main text. Blue shaded regions denote where gravity waves propagate, red shaded regions are where acoustic waves propagate, and gray regions represent evanescent zones.
Paper: The Mg–K Anticorrelation in ω Centauri
Authors: Deimer Antonio Alvarez Garay, Alessio Mucciarelli, Carmela Lardo, Michele Bellazzini, and Thibault Merle
Figure caption: Color–magnitude diagram of ω Centauri. Black points represent all the targets of ω Centauri observed with Gaia, while the targets selected for this study are colored according to their metallicity. The color scale is shown on the right side.
Paper: The Mg–K Anticorrelation in ω Centauri
Authors: Deimer Antonio Alvarez Garay, Alessio Mucciarelli, Carmela Lardo, Michele Bellazzini, and Thibault Merle
Figure caption: Left panel: behavior of [K/Fe] as a function of [Mg/Fe]. Each star is color coded according to its value of [Fe/H], and the color scale is shown on the right side. The error bar represents the typical error associated with the abundance ratios. The distribution of [K/Fe] and [Mg/Fe] are shown as marginalized histograms. Right panel: the same as the left panel, but for the [K/Fe] and [Na/Fe] abundance ratios.
Paper: The Mg–K Anticorrelation in ω Centauri
Authors: Deimer Antonio Alvarez Garay, Alessio Mucciarelli, Carmela Lardo, Michele Bellazzini, and Thibault Merle
Figure caption: Left panel: behavior of [K/Fe] as a function of [Mg/Fe] with the inclusion of the K-rich star 43241_J10 (red triangle). The black square represents the reference star 41375_J10 with similar atmospheric parameters to the K-rich star. Right panel: comparison between the GIRAFFE spectra of the two stars around the strong K line at 7699 Å. The large K enhancement of 43241_J10 is clearly visible from this comparison.
Paper: The Mg–K Anticorrelation in ω Centauri
Authors: Deimer Antonio Alvarez Garay, Alessio Mucciarelli, Carmela Lardo, Michele Bellazzini, and Thibault Merle
Figure caption: Run of the [K/Fe] abundance against [Mg/Fe] for stars in GCs. ω Centauri stars are shown as red circles. Stars in NGC 2808 are plotted as green circles (Mucciarelli et al. 2015), whereas stars in NGC 2419 are in blue (data from Mucciarelli et al. (2012) and Cohen & Kirby (2012) are shown as circles and squares, respectively). The dashed line splits the Mg-poor from the Mg-rich stars.