adsabs/AstroCLIMB huggingface dataset:
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an out-of-plane recoil kick. The face-on, postkick distribution of stars at t = 0 (left), t = 0.15 Myr (center), and t = 0.75 Myr (right). Bound and unbound stars are shown with blue triangle markers and green dots, respectively. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The recoil kick direction is out of the plane, marked and labeled as v kick. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. Both the bound and unbound populations seem to expand radially over time.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an in-plane recoil kick. The postkick surface density distribution of bound stars in the face-on (top) and edge-on (bottom) orientations at t = 0 (left) and t = 0.5 Myr (right), where the stars have been separated into prograde (blue contours) and retrograde (orange contours). The “o” marker shows the recoiling black hole, and density contours are calculated in the frame comoving with the black hole. In each orientation, the recoil kick direction is marked and labeled as v kick. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The density contours reveal a prograde eccentric disk and an antialigned retrograde disk forming a bar-like structure.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The composite MDF for all UFDs in our sample, shown against select UDF MDFs from the literature. (Left) A breakdown of the composite MDF by contribution from each UFD in our sample. (Right) Our MDF (red) compared to those in the literature. The maroon line represents the composite MDF made from all literature measurements available for the same galaxies as those in our sample, including stars not observed by our program. Our program increases the number of stellar metallicities in these galaxies by nearly a factor of 5. The gray line represents the composite UFD MDF made from all available UFD stellar metallicity measurements compiled by Simon (2019). Our work more than doubles the number of metallicities in all UFDs. There is a significant increase in the number of extremely metal-poor star candidates in these systems compared with previous studies. In all cases, our work demonstrates the excellent ability for space-based CaHK narrowband imaging to significantly expand the number of UFD stars with metallicity measurements.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The mass–metallicity relation for dwarf galaxies, updated with results from this work. (Left) We add our 〈[Fe/H]〉 measurements to the 〈[Fe/H]〉 measurements of other MW dwarf galaxies, using the table compiled by Simon (2019). Our results show a clear floor in the mass–metallicity relation in the UFD regime. We characterize this putative floor using only our measurements, assuming that the floor can be described by a Gaussian mean and scatter, placing the mean of the floor at [Fe/H] = −2.61 ± 0.08 dex. (Right) Our 〈[Fe/H]〉 measurements compared to those from select cosmological simulations. While simulations can broadly reproduce the mass–metallicity relation for the more luminous dwarf galaxies, they currently struggle to enrich less-luminous dwarf galaxies to the same level as we observe.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: A gallery of CaHK diagrams for each UFD, ordered by decreasing luminosity. We have overplotted the MIST ﹩\unicode{x00251}﹩-enhanced ([α/Fe] = +0.40) CaHK tracks for RGB stars in most cases and MS tracks for Ret II, Wil 1, Seg 1, and Dra II, which are dominated by MS and MSTO stars. The tracks have been convolved with ASTs run for each galaxy. These tracks are solely for illustrative purposes to demonstrate the impact of ASTs, and actual tracks used for fitting individual stars may look different due to the process described in Section 3.1. It is clear from the distribution of stars that each galaxy hosts stars over a wide range of metallicities.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: A gallery of MDFs for each galaxy based on our CaHK fitting. Metallicity bin sizes are 0.4 dex wide, which is comparable to typical stellar metallicity uncertainties. Well-constrained fits are indicated by shaded gray regions, whereas poorly constrained fits—largely upper limits—are shown as open histograms. We overplot the MDFs with the best-fit Gaussian (red). With the exception of Ret III, we resolve σ [Fe/H] above at least the 2σ level for our UFD sample.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The potential impact of foreground contamination on our results illustrated using Ret II. (Left) CMD of the TRILEGAL foreground model (Vanhollebeke et al. 2009) by querying 0.5 deg2 centered around Ret II, color coded by metallicity. Middle: remaining MW foreground stars (colored) from applying the same isochrone cut used to select Ret II members. (Right) Impact of foreground contamination when scaling down the number of expected interlopers by the WFC3 FoV. We typically expect ∼1 MW interloper in our final stellar sample. The nature of our observations and selection criteria combine to make foreground contamination minimal.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The effect of unresolved binaries on the CaHK color. The y-axis shows the difference in CaHK color between a single MS star at 0.7 M ⊙ and a binary system composed of a 0.7 M ⊙ MS star with companions from 0.1–0.7 M ⊙, for different metallicities spanned by our CaHK color grid. The impact of binary stars on our metallicities is small-to-modest compared to other sources of uncertainty.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: A gallery of F606W–F814W CMDs with membership selection indicated by the orange boxes drawn around the RGB. After making this initial selection, we crossmatch against literature radial velocity data where available to remove foreground interlopers. Stars used to infer MDFs are color coded with F395N S/N >10.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: We compare our σ [Fe/H] measurements, made assuming a Gaussian characterization of the MDF, to the σ [Fe/H] measurements of other MW dwarf galaxies (compiled by Simon 2019). Our results confirm the large internal metallicity variations in these systems.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The mean metallicities of our UFDs compared to those of recent streams characterized by S5 (Li et al. 2022) and Pristine (Martin et al. 2022). The distributions are noticeably different, suggesting UFDs are not the main progenitors of the currently known MW stream population.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. Top: the postkick distribution of the z-component of the angular momentum (normalized by the circular angular momentum at a given radius) as a function of postkick semimajor axis scaled by the characteristic radius, with the color bar showing the y-component of the eccentricity vector. We show radii corresponding to the circular orbits illustrated in the schematic Figure 1, A, B, and C (black dashed lines), and the corresponding postkick distribution emanating from those radii (pink, orange, and green solid lines, respectively). Second from top: two measures of the postkick apsidal alignment: the magnitude of the mean eccentricity vector (blue solid line), ∣〈 e 〉∣, and the mean unit eccentricity vector (orange dashed line), ﹩| \langle \hat{e}\rangle | ﹩, binned by semimajor axis. The shaded noise floor shows the maximum expected deviation from 0 (at the 3σ level) for an isotropic distribution. Second from bottom: the eccentricity profile as a function of semimajor axis color coded by orbital inclination. Bottom: the retrograde fraction of the disk as a function of semimajor axis. The postkick stellar orbits exhibit a rich structure of apsidal alignment, eccentricity, and retrograde fraction each with a sensitive dependence on the semimajor axis.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. A schematic diagram illustrating four pre- and postkick orbits. Left: initial circular orbits A, B, and C with markers indicating the stars’ positions at the time of kick, and the arrow labeled v kick is the black hole kick direction. The stars initially move on counterclockwise (prograde) orbits. Right: the postkick eccentric orbits where dashed lines indicate where the stars move on clockwise (retrograde) orbits. Thus, we expect a retrograde population to emerge above a certain radius in the postkick stellar distribution.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. The face-on, postkick distribution of stars at t = 0 (top left), t = 0.15 Myr (top right), and t = 0.75 Myr (bottom). Bound stars are separated into prograde (blue triangle markers) and retrograde (orange “+” markers). The unbound stars are marked with green dots. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The arrow labeled v kick indicates the recoil kick direction. All positions are shown in the galactic center frame. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The prograde, bound orbits form an END in the +y-direction. The unbound stars form an arc of overdensity behind the recoiling black hole.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. The postkick surface density distribution of bound stars in the face-on (top) and edge-on (bottom) orientations at t = 0 (left) and t = 0.1 Myr (right), zoomed in to subparsec scales. On this scale, all stars are on prograde orbits. The recoil kick direction is marked in each orientation and labeled as v kick. The “o” marker shows the recoiling black hole, and density contours are computed in the reference frame of the recoiling black hole. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The postkick density contours reveal an END.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. Pre- and postkick number density as a function of apoapsis distance, r + (normalized to r  c  as defined in Equation (3)). The initial prekick number density is flat, but the postkick number density extends to higher apoapsis distances with a turn around from a flat region to a power-law region around r + ≈ 4. At r + ≳ 4, the number density is roughly distributed as N ∝ r −0.93 according to our linear fit.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Variation of escape flux of different ion species along x = −2R  V  during the solar wind pressure pulse event.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Density of O2 + in logarithmic scale and tailward velocity along x = −2R  V  at 1 and 2 hr.
Paper: Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Figure caption: Contour plots of escape flux of different ion species in the x–y plane.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Left panel: evolution over time of the power spectral hue (blue points) and spectral hardness (pink points) for the 2007 full outburst. The vertical brown and gray lines and shaded region indicate the best-fitting values and 1σ contours for t hue,trans and t hr,trans, respectively, and the shaded region indicates the uncertainty on the model fits. The four arrows indicate the four observations we model in Section 3. Right panel: identical plot for the 2009 HS outburst.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Power spectra of the four epochs highlighted in Figure 2. The top left observation was taken at the start of the outburst, the top right immediately before t hue,trauns, the bottom left between the transition times t hue,trauns and t hr,trauns, and the bottom right immediately after t hr,trauns. The vertical lines indicate the frequency bounds used to compute the power spectral hue. Dashed–dotted lines indicate the zero-centered Lorentzian and dashed lines the broad Lorentzian used to model the broadband noise. Dotted lines indicate the narrow Lorentzians used to model the QPOs. The solid lines represents the total model.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Example of the hue evolution. The purple cross indicates the central point at (PC1, PC2) = (4.51920, 0.453724), and the dashed gray line the line is the reference from which the hue angle is calculated. The scarlet diamond, near (PC1, PC2) = (1, 1), corresponds to the low HS. The blue cross, at (PC1, PC2) = (30,0.1), corresponds to the HIMS.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Evolution of the power spectral hue and spectral hardness for the 2002, 2004, 2006, 2008, and 2010 outbursts of GX 339. The color coding is identical to Figure 2.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Time-averaged energy spectra of the four epochs highlighted in Figure 2. Dashed lines indicate the continuum, dashed–dotted lines indicate the reflection, and continuous lines indicate the total model.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: Difference in transition times for each full outburst of GX 339−4 against the 3–30 keV count rate at the transition times t hue,trans (top panel) and t hr,trans (bottom panel). The error bar for the count rate is smaller than the symbols. Brighter outbursts tend to show quicker state transitions.
Paper: Variability as a Predictor for the Hard-to-soft State Transition in GX 339−4
Authors: Matteo Lucchini, Marina Ten Have, Jingyi Wang, Jeroen Homan, Erin Kara, Oluwashina Adegoke, Riley Connors, Thomas Dauser, Javier Garcia, Guglielmo Mastroserio, Adam Ingram, Michiel van der Klis, Ole König, Collin Lewin, Labani Mallick, Edward Nathan, Patrick O'Neill, Christos Panagiotou, Joanna Piotrowska, Phil Uttley
Figure caption: The iron line profile in the four epochs highlighted in Figure 2, shown as the ratio to a Comptonization model. The color coding is identical to Figure 3. We only show the 3–11 keV band for clarity.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: Histogram of minor branch halo masses m above, measured at z above, the lowest redshift (latest time) at which the branch exceeded the cooling threshold mass for V cut = 30 and 40 km s−1, in orange and blue, respectively. The dotted lines show the corresponding threshold masses for star formation at z reion = 10. Dashed and solid lines correspond to minor branches that cross the threshold before and after z reion, respectively. The bimodality arises because there is a population of halos that exceeds the threshold before reionization at z reion but not afterward. The sharp lower mass limit corresponds to the least massive halos that exceed the threshold at z reion. The gap is created by the large instantaneous increase in the threshold at z reion (see Figure 2) as explained in the text.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: Stellar mass surface density profiles for the most massive ghost galaxies, predicted with our particle tagging prescription (gray lines) for V cut = 30 km s−1 (solid) and V cut = 40 km s−1 (dashed). Gray circles and squares mark the respective half-light radii of these profiles. Left and right panels show results with particle tagging most bound faction parameters of 1% and 10%, respectively. In both panels, the colored lines show profiles for a selection of real LSB dwarf galaxies as given in the legend; a description of these data and references are given in the text. The crosses mark the half-light radii of the dwarfs. The half-light radius of Tucana B is ∼80 pc, outside the range of radii shown.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The stellar mass function of ghost galaxies for our V cut = 30 km s−1 model, assuming that 1% of available baryons are converted to stars at z above. Colors show the contribution of different bins of present-day virial mass, in the range 109–1010 M ⊙. The bimodality follows directly from the distribution of m above shown in Figure 6.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The effects of changing V cut from 30 km s−1 (orange line, repeating Figure 4) to 40 km s−1 (blue line). A higher cooling threshold increases the peak fraction of ghost galaxies (to, e.g., ∼20% of all halos at ≈8 × 109 h −1 M ⊙) and broadens the mass range of hosts.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The z = 0 stellar mass function of ghostly galaxies (dashed black line) for our V cut = 30km s−1 model assuming the SMHM relation of Behroozi et al. (2019). Solid lines separate the contributions from galaxies comprising only one ghost (blue) and those formed by the merging of multiple ghosts (orange). The typical ghost stellar mass is reduced compared to the assumption of a constant galaxy formation efficiency in Figure 8.