adsabs/AstroCLIMB huggingface dataset:
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Collapse evolution for a representative stellar model, 250.25, with the typical rotation parameters p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm. Top: fallback rates ﹩{\dot{M}}_{\mathrm{fb}}﹩ onto the BH (blue; direct), onto an accretion disk (yellow), and in total (green), as a function of the total cumulative collapsed mass M fb. The dotted lines indicate the corresponding evolution when ignoring the effect of a jet. Center and bottom: evolution of the angular momenta (center) and masses (bottom), as determined by Equations (9)–(14).
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Top: the accretion rate at which the ejecta are being produced as a function of the cumulative ejecta mass for model 250.25, with p = 4.5, f kep = 0.3, and r b = 1.5 × 109 cm. The nucleosynthesis regimes according to Equation (26) are color-coded (from top to bottom, in the same order as in Equation (26)). The red dashed line indicates the cumulative mass ejected until t = t diss (see below). Bottom: the corresponding mass fractions of 56Ni synthesized in disk outflows and 4He in the accretion disk. The production of 56Ni sets in at around ≈ 10 s, when the accretion rate enters the light green regime in the top panel (the fourth accretion regime in Equation (26)). The vertical dashed line indicates the time t diss at which only 50% of the α-particles are dissociated in the disk. For t > t diss, we ignore further 56Ni production in the outflows.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: BH masses and disk wind ejecta properties across the parameter space of progenitor rotational profiles (envelope Keplerian fraction f K and break radius r b, p = 4.5; see Figure 1, bottom panel) for model 250.25. The final BH mass (top), the total ejected mass in heavy (A > 136) r-process elements, including lanthanides (center top), the light (A < 136) r-process material (center bottom), and 56Ni (bottom) are shown. The red contours indicate the inferred primary mass of GW190521, together with its 90% confidence limits (﹩{85}_{-14}^{+21}\,{M}_{\odot };﹩ Abbott et al. 2020). The cyan contours delineate the final BH masses of 60 M ⊙ and 130 M ⊙, which approximately correspond to the lower and upper end of the PI mass gap.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Properties of the stellar models at the onset of collapse, showing the enclosed mass as a function of stellar radius (top: models E15 and E20 of Heger et al. 2000; center: models 200.0 and 250.25 of Renzo et al. 2020b), with an example of the imposed specific angular momentum profile for model 250.25, with p = 4.5, r b = 1.5 × 109 cm, and f K = 0.3 (see Equation (2)), compared to the corresponding Keplerian profile (solid green line; bottom). The light (dark) shaded region in the top panel represents the hydrogen envelope of the E20 (E15) model. Such envelopes are absent from the models of Renzo et al. (2020b).
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Scan of the parameter space for model 250.25, setting p = 4.5. We show the mass fractions of lanthanides (top), the heavy r-process elements (A > 136; center top), the light r-process elements (A < 136; center bottom), and 56Ni (bottom) in the ejecta, assuming the full mixing of ejecta components. The red contours indicate the inferred primary mass of GW190521, together with its 90% confidence limits. The cyan contours delineate final BH masses of 60 M ⊙ and 130 M ⊙, which approximately correspond to the lower and upper end of the PI mass gap.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The flux per unit wavelength at bolometric peak for each of the five models defined in Table 2. All of the spectra have broad absorption features that are consistent with high-velocity outflows, and low-temperature pseudo-blackbody spectra, which are consistent with high-opacity compositions. These spectra distinguish superKNe from the other classes of SNe, which are much bluer, and from other dust-enshrouded explosions, in which broad absorption features are absent.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The bolometric light curves of the models in Table 2, compared to the prototypical SNe 2011fe (Type Ia), 2002ap (Type Ic-bl), 2013ab (Type II-p), and 2018zd (electron-capture). The superKN light curves are dimmer than the SNe Ia ones, but at some epochs they can approximate the light curves of SNe Type Ic-bl and Type IIp.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Analytic light-curve estimates across the parameter space for model 250.25, setting p = 4.5. The peak luminosity (top), peak effective temperature (center), and peak timescale (bottom) are shown. The red contours indicate the inferred primary mass of GW190521, together with its 90% confidence limits. The cyan contours delineate final BH masses of 60 M ⊙ and 130 M ⊙, which approximately correspond to the lower and upper end of the PI mass gap.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: (a) Temperature–magnitude plots comparing our observed systems (consistent members = blue squares; confirmed members = blue circles; rejected members = red crosses) with known/probable members of their purported associations in the literature (open circles). Given their similar ages, our observed Upper Centaurus Lupus and Upper Scorpius candidates are plotted together, with the Upper Scorpius census of Luhman (2018) for comparison (only diskless stars are shown; Esplin et al. 2018). Literature members of β Pictoris are drawn from Shkolnik et al. (2017) and those of Columba and AB Doradus Major from Gagné et al. (2018). Baraffe et al. (2015) isochrones at 1, 10, 50, 120, and 500 Myr are also plotted for comparison. All magnitudes have been dereddened with the method described in Section 3.3 or with extinction values in the literature reference, if available. (b) Temperature–magnitude plots comparing our observed systems (consistent members = blue squares; inconclusive members = blue question marks; rejected members = red crosses) with known/probable members of their purported associations in the literature (open circles). Literature members of Carina-Near are drawn from Gagné et al. (2018) and those of Coma Berenices from Gagné et al. (2018) and Tang et al. (2019). Baraffe et al. (2015) isochrones at 1, 10, 50, 120, and 500 Myr are also plotted for comparison. All magnitudes have been dereddened with the method described in Section 3.3.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Probability of membership in the proposed association vs. systemic velocity, also represented as the mass ratio of the red component to the blue component, for all spectroscopically resolved binaries in our sample. Each mass ratio was taken together with the measured stellar component RVs to calculate a systemic velocity, which was then fed into BANYAN Σ. The association corresponding to the membership probability is labeled within each plot. Note that J0441−1523 and J0703−1723 are also resolved binaries, but they are not depicted here because their association membership probabilities are zero for all possible systemic RVs.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Equivalent width of Hα (left) and Li λ6707 (right) vs. effective temperature for all systems in our observed sample where the associated spectral line is detected. Lines in absorption correspond to positive equivalent widths (note the flipped y-axis for Hα). Circles mark systems that we confirmed as members of their purported association, squares mark systems found consistent with association membership, and crosses mark systems whose membership we reject. Systems are color-coded by the age of their association (as per Table 1). For Li λ6707, we also plot the equivalent widths of confirmed members from the literature for comparison, with black filled circles corresponding to β Pictoris members (Shkolnik et al. 2017) and open circles corresponding to AB Doradus Major (Mentuch et al. 2008). The points marked with a white cross (J0331−1525 and J1515−2527) are tentative detections. Nondetections are not displayed; some error bars are too small to be visible.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: BANYAN Σ membership probability curves plotted over the CCF of each spectroscopically unresolved or ambiguous binary in our sample. The association(s) corresponding to the membership probability curves is labeled within each plot. Note that “ARG” refers to Argus, a 40–50 Myr old association that is not discussed in this paper (Zuckerman 2019).
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: BANYAN Σ membership probabilities recomputed taking into account our measured RVs vs. those as originally reported in Gagné & Faherty (2018). Only the nonbinary candidate members whose revised probabilities still most favor membership in their originally proposed association (i.e., as opposed to the field) are shown. Marker shape corresponds to whether spectral line diagnostics confirmed youth (filled circles), rejected it (crosses), or were consistent with membership (open squares). Gray dashed line of unity provided for comparison.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: RVs presented in this paper vs. those from Gaia DR2, for the 14 systems in our observed sample with such Gaia data available. The three stars with RV measurements that do not overlap within 1σ are marked in red; all three overlap within 1.5σ. FGK stars are plotted with circles, and M stars as only 1σ error bars. Dashed line of equality included for comparison.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Final estimates of the effective temperatures of the targets in our observed sample, compared to values reported by Muirhead et al. (2018), Gagné & Faherty (2018), Anders et al. (2019), and Cifuentes et al. (2020). All binary systems are excluded.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Remnant mass vs. ZAMS mass for different IFMRs. The Raithel18 IFMR is defined for solar metallicity only. The Spera15 and SukhboldN20 IFMRs are a function of metallicity; in this figure they are evaluated at four different metallicities corresponding to the values described in Section 2.3. The dashed black line at 3 M ⊙ represents the BH/NS boundary. While the Spera15 IFMR is analytic, the SukhboldN20 and Raithel18 IFMRs are stochastic. Even stars with high ZAMS masses can form NSs instead of BHs. The differences in the IFMRs are most apparent at the highest stellar and compact object masses.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Top: the SukhboldN20 black hole (BH) initial–final mass relation at several different metallicities. Below M ZAMS ≲ 40 M ⊙, the BH remnant masses are identical independent of metallicity. Bottom: the probability of BH formation at several different metallicities. Below M ZAMS ≲ 60 M ⊙, the probabilities are identical independent of metallicity.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Mass distributions of all compact objects (WD, NS, BH) produced by each IFMR. The population synthesis was performed over an area of 0.34 deg2 centered on the coordinates of the OGLE-IV-BLG611 field. The histograms show the underlying population of compact objects, i.e., lensing is not considered. The WD mass distributions are nearly identical for all three IFMRs except at the high-mass end where Spera15 has an excess of high-mass WDs as compared to SukhboldN20 and Raithel18. The NS mass distributions are similar for SukhboldN20 and Raithel18, while Spera15 has significantly more high-mass NSs. The BH mass distribution varies greatly depending on the IFMR.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: The distribution of [Fe/H] at two different Galaxia field locations. Vertical black lines demarcate the chosen metallicity binning for the SPISEA clusters run with a metallicity-dependent IFMR, with the metallicity assigned to each bin labeled in red. Note that for the Raithel18 IFMR all SPISEA clusters are solar metallicity only.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Top: evolution with redshift of the virial temperature of the halos. The horizontal dashed gray line shows T = 104 K, the limit for atomic cooling in halos. The vertical dashed gray line shows the approximate timing of reionization when all halos halt their SF. For comparison, we also plot the IGM temperature. Bottom: evolution with redshift of the virial mass of the halos. The opacity of the lines indicates when SF is ongoing (full) or quenched (opaque). For comparison, we plot the model of Benitez-Llambay & Frenk (2020) as a solid black line. The horizontal gray dashed line indicates the Population III enrichment threshold in our model (before reionization), while we show the atomic cooling threshold of 104 K for z < 7.7. The vertical gray dashed line denotes the quenching redshift of z = 7.7.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Fraction of BH events compared to total events in the OGLE-like survey sample as a function of t  E . The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The SukhboldN20 IFMR produces the fewest BHs and has the lowest fraction of BH events at long t  E  (>100 days). The Spera15 IFMR produces the most BHs and has the highest fraction of BH events at long t  E . Regardless of IFMR, roughly at least a third of events with t  E  > 150 days are BH lenses.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Each of the four figures shows three panels as a function of time for one simulation, respectively: the top panels show gas density within 40 pc (solid colored) and within R 200 (black line). The middle panels show the cooling time measured within the virial radius (colored), the dynamical time of the halo (black), and the Hubble time (dotted). The bottom panels show the net mass flow rate (outflow rate minus inflow rate) across the spherical shell with radius R 200 and width 0.1 R 200. The gray bands in each panel indicate when SF is ongoing. The black vertical dashed line shows the time of quenching (z = 7.7), which is just after the central reionization redshift (z = 7.8).
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Comparisons of the present-day black hole (BH) mass function of the Milky Way produced using star formation history and metallicity from the Galaxia simulation and the Raithel18, Spera15, and SukhboldN20 IFMRs of SPISEA with the astrophysical BH mass function generated from the LIGO-Virgo-KAGRA GWTC-3 results (The LIGO–Virgo–KAGRA Collaboration et al. 2021) using their Power Law+Peak model (Abbott et al. 2021). The four spikes in the Spera15 IFMR present-day BH mass function are artifacts of the metallicity binning scheme in the population synthesis procedure described in Section 2.3. Finer metallicity bins would remove these artificial spikes at the expense of increased computational time.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Fraction of BH events compared to total events in the OGLE-like survey sample as a function of π  E . The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. Because the Spera15 IFMR produces more massive BHs than Raithel18 and SukhboldN20, it has the highest fraction of BH events at small π  E  (<0.02). Although the SukhboldN20 IFMR produces more massive BHs than the Raithel18 IFMR, it also produces fewer BHs overall, so the fraction of BH events at small π  E  for those two IFMRs are similar.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: SFH in bins of 10 Myr (thin lines) and 500 Myr (thick lines). On the left the x-axis is redshift, while on the right it is look-back time in Gyr. Halo A and Halo D restart SF around z = 5. Halo B and Halo E remain quenched after reionization. The gray bands in each panel indicate the time of hydrogen reionization.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Inferred neutron star masses for source type using relativistic pulsar timing and Doppler spectroscopy. The upper mass limit obtained from the DNS GW170817 is shown in red (Margalit & Metzger 2017). Error bars indicate a 90% confidence interval.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Mock V-band surface brightness maps for each simulation at z = 0. Each image is 1.4 kpc × 1.4 kpc. Notice that the color bar is rescaled for each image. The simulation is not rotated, only repositioned to place the halo in the center.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Top: discovery light curve of 2M1222−57 from TESS FFI observations of sectors 10 and 11 (see Bouma et al. 2019). (Bottom: light curve phase folded on a period of 3.071 days with (right) and without (left) out-of-eclipse variations removed. Note that the out-of-eclipse variations include both a periodic modulation with peak-to-peak amplitude of ∼0.075 mag and an additional, more stochastic, source of variability at the level of ∼1%.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: TESS 2 minute cadence light curve from Sectors 37–38. Top: points in eclipse have been removed to isolate the out-of-eclipse variations. Middle: phase folded on the orbital period after smoothing out the out-of-eclipse variations. Bottom: same as middle, but binned by 30  min for comparison with Sectors 10–11 (Figure 4).
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Phase-folded TESS FFI light curve from Sectors 10–11 (Figure 1) after smoothing out the out-of-eclipse variations.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Spatial map of LCC and its proper motions (from McBride et al. 2021) color coded by the inferred age and parallax respectively. System 2M1222−57 is highlighted against LCC with a larger circle with black outline.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Gala color–magnitude diagram of LCC (from McBride et al. 2021) in black, and 2M1222−57 marked by the yellow circle.