adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Origin of Stars on Bound and Unbound Orbits Causing Tidal Disruption Events
Authors: Shiyan Zhong, Kimitake Hayasaki, Shuo Li, Peter Berczik, Rainer Spurzem
Figure caption: Radial profiles of the density (left) and of the square of the stellar velocity dispersion (middle) for the model cluster with M BH = 0.01. In the left panel, the red dots and gray solid line represent the simulated and numerically fitted density profiles, respectively. In the middle panel, the red dots and gray solid line denote the square of the stellar velocity dispersions evaluated by the simulation and by Equation (21), i.e., the Jeans equation, respectively. The right panel depicts the apocenter distance radius r  a  as a function of the specific orbital energy E(=v 2/2 − GM BH/r) for a radial orbit with zero angular momentum. The horizontal blue dotted line indicates the influence radius r h, whereas the vertical black dotted line corresponds to the line of E = 0.
Paper: Exploring the Origin of Stars on Bound and Unbound Orbits Causing Tidal Disruption Events
Authors: Shiyan Zhong, Kimitake Hayasaki, Shuo Li, Peter Berczik, Rainer Spurzem
Figure caption: Dependence of Q on the apocenter distance radius r a for bound stars. Hénon units are adopted for the plot. The solid ocher line and horizontal black dotted line delineate the ﹩-\mathrm{ln}{{ \mathcal R }}_{\mathrm{lc}}﹩ curve (see Magorrian & Tremaine 1999 for details) and the Q = 1 line, respectively, which provides the criterion for distinguishing the empty and full loss-cone regimes. The vertical dotted red line represents the influence radius of the SMBH. The solid black and light blue lines indicate the Q curves with Q boost = 1 and Q boost = 5, respectively, which are given by applying the fitted simulation results to Equation (19).
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The recovery of the BAO angular scale θ BAO with BNS merger events (for a 3G detector network) centered around different values of D  L  in shells of about ∼150h −1 Mpc. The solid continuous curve represents the relation between θ BAO and luminosity distance D  L  to the shell for the ΛCDM model used in simulations using parameters from the Planck 2018 results (Aghanim et al. 2020).
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The one-dimensional marginalized posterior distribution of the Hubble parameter H 0 = 100h km s−1 Mpc−1 using the angular BAO scale measurements θ BAO from simulated GW events with the 3G detector network in three shells centered at D  L  ∼ 1000, 1300, and 1600 Mpc. The injected value is shown by the dashed vertical line. The three cosmological models used here are described in Table 1. The left panel shows GW-BAO+CMB constraints and the right panel shows constraints from the GW-BAO+CMB+EM counterpart.
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The combined constraints (GW-BAO+SDSS-BAO+CMB) on the w 0 w  a  CDM model with BAO measurements from GW localization volumes (from simulations) and CMB/BAO constraints from the galaxy surveys. For the marginalized one-dimensional posteriors, we show 68% bounds with the median value. For two-dimensional contours, we show 60% and 90% regions. The injected values are shown by blue lines corresponding to the ΛCDM model with parameters consistent with the Planck 2018 results (Aghanim et al. 2020).
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The combined constraints (GW-BAO+SDSS-BAO+CMB) on the wCDM model with BAO measurements from GW localization volumes (from simulations) and CMB/BAO constraints from the galaxy surveys. For the marginalized one-dimensional posteriors, we show 68% bounds with the median value. For two-dimensional contours, we show 60% and 90% regions. The injected values are shown by blue lines corresponding to the ΛCDM model with parameters consistent with the Planck 2018 results (Aghanim et al. 2020).
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The GW-BAO+EM counterpart constraints on the Hubble parameter H 0 = 100h km s−1 Mpc−1 and comoving BAO scale r  s  [Mpc] for the ΛCDM model with BAO measurements from GW localization volumes (simulations). For the marginalized one-dimensional posteriors, we show 68% bounds with the median value. For two-dimensional contours, we show 60% and 90% regions. The injected values are shown by the blue lines.
Paper: Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Authors: Sumit Kumar
Figure caption: The combined constraints (GW-BAO+SDSS-BAO+CMB) on the ΛCDM model with BAO measurements from GW localization volumes (from simulations) and CMB/BAO constraints from the galaxy surveys. For the marginalized one-dimensional posteriors, we show 68% bounds with the median value. For two-dimensional contours, we show 60% and 90% regions. The injected values are shown by blue lines.
Paper: Constraining a Companion of the Galactic Center Black Hole Sgr A*
Authors: Clifford M. Will, Smadar Naoz, Aurélien Hees, Alexandria Tucker, Eric Zhang, Tuan Do, Andrea Ghez
Figure caption: Bounds on the mass and semimajor axis of a companion IMBH in an orbit with e  c  = 0.6. Red: bounds from ∣d  j /dt∣. Blue: bounds from ∣d ϖ/dt∣. Dotted lines denote bounds on an inner companion purely from quadrupole perturbations of ∣d  j /dt∣ and ∣d ϖ/dt∣. The regions labeled “a,” “b,” and “c” are discussed in Section 2.4. The tan area denotes a gravitational-wave damping timescale for the companion shorter than 107 yr.
Paper: Constraining a Companion of the Galactic Center Black Hole Sgr A*
Authors: Clifford M. Will, Smadar Naoz, Aurélien Hees, Alexandria Tucker, Eric Zhang, Tuan Do, Andrea Ghez
Figure caption: Bounds on a companion IMBH from numerical simulations. The gray scale represents the posterior probability density distribution for the mass of the SMBH companion (m  c ) and its semimajor axis (a  c ) marginalized over the other 21 fitted parameters and normalized to 1. The scale of shades at the right of the figure indicates the relative probability. White regions are excluded. The black dashed line corresponds to the 95% confidence area. The blue curves are the same as in Figure 2. The dotted green curve corresponds to a a  c  ∼ 1/m  c  behavior. The tan area is excluded (more precisely is not relevant) as a result of gravitational-wave damping for the companion.
Paper: Constraining a Companion of the Galactic Center Black Hole Sgr A*
Authors: Clifford M. Will, Smadar Naoz, Aurélien Hees, Alexandria Tucker, Eric Zhang, Tuan Do, Andrea Ghez
Figure caption: Comparison between the results of this paper and an analysis by the GRAVITY Collaboration et al. (2023). The left panel corresponds to an inner companion, and the right panel to an outer companion. The shaded blue regions denote companion solutions with 39%, 86%, and 99% confidence, from dark to light, respectively. White regions are excluded. The dashed red curves show our analytic bounds (taken from Figure 2) for purely quadrupole perturbations. The dashed green curve (taken from Figure 3) is a rough fit to our numerical results for low-mass inner companions. Above and to the right of both curves in the left panel, we predict no companions. Between the two dashed red curves in the right panel, we also predict no companions. Background figure reproduced from GRAVITY Collaboration et al. (2023) via Creative Commons CC-BY 4.0 license.
Paper: Constraining a Companion of the Galactic Center Black Hole Sgr A*
Authors: Clifford M. Will, Smadar Naoz, Aurélien Hees, Alexandria Tucker, Eric Zhang, Tuan Do, Andrea Ghez
Figure caption: A hierarchical three-body system consisting of the Sgr A*–IMBH binary and the star S0-2. The binary can be either inside or outside the orbit of the star.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: IRSF/SIRIUS three-color composite image of M17, with J-band data shown in blue, H-band data in green, and K  s -band data in red. Image credits: Jiang et al. (2002). Superimposed are telescope/instrument apertures from ISOCAM (pink), ISO-SWS (red), and Akari (purple) observations. The two JWST apertures are shown and labeled in black. The translucent colored patches mark Spitzer-IRS spectral map observations, where each patch represents one of four distinct emission zones identified through hierarchical clustering (see Boersma et al. 2018).
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Three-color composite Subaru image of part of NGC 1333-SVS3. Here the blue channel is taken from ﹩{i}^{{\prime} }﹩-band, the green from J-band, and the red from K-band data. Image credits: SONYC Team/Subaru Telescope. Superimposed are apertures from ISOCAM (pink) and ISO-SWS (red) observations. The translucent colored patches mark Spitzer-IRS spectral map data, where each color represents one of four zones identified through hierarchical clustering (see Boersma et al. 2016). The JWST aperture is shown and labeled in black.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: Estimates of the number of serendipitous observations expected per year for transients with a variety of different instruments based on the volumetric rates of the phenomena and the observing volume of each instrument. The comoving depth out to which each instrument can observe each class of phenomenon is calculated based on the peak observed luminosity of each phenomenon, making the assumption that we have already detected the most intrinsically luminous signal from each type of transient. We take rates from Stone & Metzger (2016), Coppejans et al. (2020), Margutti & Chornock (2021), and Ghirlanda & Salvaterra (2022). For the GRBs, both long and short, we apply a beaming correction assuming a jet opening angle ∼3°. See Table 3 for more details. As with the rest of the paper, the number of expected observations per year is quoted out to z = 1, corresponding to d  L  ∼ 6700 Mpc or d com ∼ 3350 Mpc. For each class of transient shown here, next-generation instruments (open markers) represent an increase in the anticipated number of events observed per year. In the case of more intrinsically luminous transients, this is due to increased FOV, while less luminous classes benefit more from improved sensitivity (see Figure 8).
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: To decouple the advantages of increased FOV and sensitivity, we show extragalactic transient rates (Stone & Metzger 2016; Coppejans et al. 2020; Margutti & Chornock 2021; Ghirlanda & Salvaterra 2022) as a function of FOV with a fixed flux limit (left, sensitivity = 10−13 erg s−1 cm−2) and the same rates as a function of sensitivity with a fixed FOV (right, FOV = 1 deg2). As in the rest of this work, we limit the rates to z ≤ 1—which is why the number of observations per year eventually flattens with increasing sensitivity. For luminous sources, like those included here, substantial increases in the number of events detected within z ≲ 1 will primarily come from instruments with increased FOV.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: The maximum distance out to which each instrument can observe different classes of transient/variable vs. the normalized FOV (by the area of the sky). As in the rest of this work, we limit to z ≤ 1 (d  L  = 6.7 × 106 kpc), which is shown by the gray dashed line. For less luminous classes of transient, the improved sensitivity from proposed/planned instruments (shown with open markers) represents an increase of up to ∼3 orders of magnitude in the distance out to which these events can be detected and observed. This significantly enlarges the potential observing volume for these signals.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: Top: a schematic illustration of the DLPS. Colored blocks cover the region where light curves of that class exist in the DLPS. The crosshatched blocks represent where we expect events of a particular class but have a paucity of observations (for SBOs, we include in this the region of the DLPS where we have candidate stellar surface SBOs). Bottom: an additional view of the DLPS, which emphasizes the phase space of individual classes of transient rather than their position in the larger transient phase space. We note that the lower panels are all scaled individually in duration and luminosity.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: The duration–flux phase space of X-ray transient and variable phenomena. To demonstrate the limitations of current observatories, we mark the 0.3–10 keV flux limit for a handful of instruments, assuming a 1 ks integration time.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption:                         (a) Continuation of Figure 4 showing the performance of SESAMME in fitting FUV spectra of YMCs. Top: the black curve shows the H I absorption-corrected, combined G130M+G160M spectrum of YMC M83-3 (Hernandez et al. 2019) from HST/COS, after smoothing and resampling to the 0.6 Å resolution of our Starburst99 models. Intervals in gray shaded regions were masked during the modeling process and include ISM emission and absorption features, chip gaps, and geocoronal Lyα and O I. The blue curve shows the median model (see the text for details), while the teal dotted curves show 50 random samples from the cleaned MCMC chain. Bottom: model residuals for the 50 samples. (b) Continuation of Figure A1 for the subsolar metallicity YMC NGC 1313-1, as modeled using BPASS (top) and Starburst99 (bottom) SSPs. (c) Continuation of Figure A1 for subsolar metallicity YMC NGC 1313-2, as modeled using BPASS (top) and Starburst99 (bottom) SSPs.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: An example of SESAMME’s performance in modeling the FUV spectrum of a metal-rich YMC. Top: the black curve shows the H I absorption-corrected, combined G130M+G160M spectrum of YMC M83-8 (Hernandez et al. 2019) from HST/COS, after smoothing and resampling to the 1 Å resolution of the BPASS models. Intervals in gray shaded regions were masked during the modeling process and include ISM emission and absorption features, chip gaps, and geocoronal Lyα and OI λ1302. The blue curve shows the median model (see the text for details), while the teal dotted curves show 50 random samples from the cleaned MCMC chain. Middle: model residuals for the 50 samples. Bottom: zoom-ins to regions that include age-sensitive features: NV λ1240 in the bottom left and CIV λ1550 in the bottom right.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: Comparison of N V λ λ1238, 1242 line profiles from BPASS v2.3 (top) and Starburst99 (bottom) models. Red and purple curves, respectively, show populations of age 2 and 5 Myr. Populations with a stellar metallicity Z=0.008 are shown as solid lines, while Z = 0.04 models are shown with dashed lines. Some models have been shifted in luminosity for visualization purposes. The vertical gray lines mark the central wavelengths of the N V doublet components. Starburst99 predicts a significant P Cygni line profile even at high metallicity and ages ∼5 Myr, while N V is seemingly absent in all but the youngest and most metal-poor BPASS models we show here.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: An example of SESAMME’s performance using SB99 models to characterize the FUV spectrum of a YMC. Top: the black curve shows the HI absorption-corrected, combined G130M+G160M spectrum of YMC M83-8 (Hernandez et al. 2019) from HST/COS, now smoothed and resampled to the 0.6 Å resolution of our SB99 models. As in Figure 4, intervals in gray shaded regions were masked during the modeling process, and teal dotted curves show either 50 random samples from the MCMC chain (top) or the residuals of those samples from the observed spectrum (middle). In the bottom panels, we show zoom-ins to age-sensitive features (NV λ1240 on the left and CIV λ1550 on the right).
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: Corner plot for the SESAMME fit to the UV spectrum of M83-8, using either Starburst99 (purple) or BPASS v2.3 (red) as the assumed model suite. This spectrum has an S/N at 1310 Å of ∼6.8 at the native 0.06 Å/resel resolution of COS (S/N ∼26.8 after binning to at the 1 Å resolution of BPASS). Red and purple dashed lines mark the median of each parameter’s PDF for the two model sets. Gray dotted lines mark the BPASS age and metallicity grid points; grid points for our SB99 models are omitted for clarity. Black solid lines mark the best-fit age and metallicity from Hernandez et al. (2019). The 2D and 1D histograms have been lightly smoothed for clarity.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: Comparison of the 16th, 50th, and 84th percentiles on the ages (left) and stellar metallicities (right) of the YMCs in M83 and NGC 1313 as determined by SESAMME (circles) and from other methods in the literature (teal triangles). For each cluster, we performed two SESAMME runs—one with BPASS v2.3 models (red) and one with Starburst99 (purple). The literature values for the M83 YMCs are from Hernandez et al. (2019), while the values for the NGC 1313 YMCs are from Sirressi et al. (2022).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Essentials of Paper I. (a) and (b) are PGs from the 10–30 keV Suzaku and NuSTAR data, respectively. They are corrected for the orbit of LS 5039, with the orbital parameters readjusted at each period (see the main text). Red/blue shows ﹩{Z}_{4}^{2}﹩ with m = 4 (left ordinate), whereas the dashed green curve gives τ 0 (right ordinate), with its search range indicated by a green arrow. (c) and (d) are background-inclusive pulse profiles, folded using the orbital solutions specified by the ﹩{Z}_{4}^{2}﹩ peak in (a) and (b), respectively. Between (c) and (d), the relative pulse phase is arbitrary.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: (a) Pulse profiles of LS 5039 from the NuSTAR data, obtained in five energy bands below 10 keV, using the same orbital solution as that used in Figure 1(d). The scale is logarithmic, to make the pulse fractions directly comparable. A yellow arrow indicates the pulse peak/bottom ratio in the 10–30 keV profile (Figure 1(d). (b) Photons detected with NuSTAR in 3.0–22.1 keV, sorted into two dimensions. The abscissa is the same pulse phase as in (a), while the ordinate is the energy in logarithmic intervals that increase by a factor of 1.33. The color coding is black–blue–purple–red–orange–yellow, from lower to higher counts.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: NuSTAR pulse significance in ﹩{Z}_{4}^{2}﹩, shown against R ppd in Equation (2). See the main text for details. (a) Results in 3–9 keV, where ﹩{Z}_{4}^{2}﹩ is in blue and τ 0 is in green. (b) The same but in 3–30 keV, shown for three values of E b; 10.4 keV (solid red), 10.7 keV (dotted black), and 10.1 keV (cyan).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Same as Figure 2 but the energy-dependent pulse-phase corrections with Equation (2) have been conducted, employing E b = 10.4 keV and R = 63 deg keV−1.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The r-band field view of GRB 220101A obtained by ALFOSC on the first night (left) and the later-time observations with HST in the F125W filter (top and bottom right). The slit direction of ALFOSC and BFOSC is also shown in the left panel of the figure as red and white rectangles, respectively. In the zoomed view of HST, the burst is circled in red and two galaxies are nearby, named G1 (R.A., decl. (J2000) = 00:05:24.83, +31:46:09.91) and G2 (R.A., decl. (J2000) = 00:05:24.77, +31:46:06.86). The burst offset to G1 and G2 is 1.″83 ± 0.″02 and 1.″38 ± 0.″02, respectively, corresponding to 12.2 ± 0.1 and 9.2 ± 0.1 kpc at a common redshift of 4.615 ± 0.001. North is up and east is to the left.