adsabs/AstroCLIMB huggingface dataset:
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Long-term optical lightcurve of CJ2056, overlaid with the SALT observations indicated by vertical, dashed green lines. The XMM-Newton, NICER, and NuSTAR observations are denoted by “X,” “Ni,” and “Nu” cyan boxes at the bottom.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: Column densities (N) as a function of virial radius normalized projected distance (d proj/R vir) for H I, O VI, C II, C III, Si II, and Si III as labeled in the top right of each panel. The sample from CUBS-Dwarfs is shown in circles and the column densities from S. D. Johnson et al. (2017) are shown as squares. Intervals with no points represent saturated systems for which we provide upper and lower limits. We color all the points black to emphasize the uniformity of the sample selection across this work and S. D. Johnson et al. (2017). The upper limits are estimated following Equation (3) and are shown as open symbols with downward arrows. H I extends far out into the IGM with decreasing detection rate and column densities. Lower ionization state metals ions show a distinct lack of extended absorption, whereas highly ionized O VI, shows a high detection rate at projected distances small than the virial radius and a nonnegligible detection rate at d proj/R vir = 1–2.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: Measured covering fractions for H I (left panels) and O VI (right panels) in six equal d proj/R vir bins for both strong absorbers (﹩\mathrm{log}N/{\mathrm{cm}}^{-2}\gt 14;﹩ top panels) and weaker ones (﹩\mathrm{log}N/{\mathrm{cm}}^{-2}\gt 13.5;﹩ bottom panels). The dark and light vertical error bars mark the 68% and 95% confidence intervals, respectively. The horizontal lines represent the d proj/R vir range contained within each bin, with each point positioned at the median d proj/R vir within the bin. We also include the covering fraction expected for random sight lines using the z < 0.7 H I and O VI column density distribution measured by C. W. Danforth et al. (2016). The gray bands around it show the 16th and 84th percentile redshifts from our survey. The H I and O VI covering fractions both decline as a function of virial normalized impact parameter.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: Example Voigt profile fits for the CGM around a dwarf galaxy with a stellar mass of ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=8.9﹩ at z = 0.1163 and d proj = 16 kpc (ID: J0154_z0.12_15). The continuum-normalized quasar spectrum is plotted in blue histogram line style with shaded bands indicating 1σ  uncertainty after rebinning by a factor of three relative to the native pixel scale for display purposes. The best fitting Voigt profile model is overplotted in a green solid line, with each individual component as dotted green lines. This example plots the system with the smallest virial radius normalized projected distance (d proj/R vir ≈ 0.16) in the sample (aside from the LLS from H.-W. Chen et al. 2020). We jointly fit the H I and the lower ionization state metal ions and separately fit C IV and O VI due to their different kinematic structures. In cases of contamination (i.e., C II 1036 Å or C IV 1550 Å), we only fit the uncontaminated line and plot the predicted absorption over the contamination.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: Left axis: The O VI masses inferred from the covering fractions in Figure 4 and 〈N O VI〉 above the cutoff, using Equation (5). The vertical red and light red bars represent the 1σ and 2σ errors inferred from bootstrapping. We find that a nonnegligible fraction of the ion mass is outside the virial radius. The point in the third bin is the mass inferred from coadding the spectra from nondetections to set an overall mass upper limit in the outer annulus. Right axis: The inferred total gas mass within each bin assuming an ionization fraction f ≈ 0.2 and a metallicity of 0.3 Z ⊙.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: (Top) The radial velocity of metal absorption components relative to the dwarf galaxy systemic velocity vs. virial radius normalized projected distance (d proj/R vir). The error bars represent ±b, the Doppler width of each component. O VI components are plotted as red points while other metal lines are shown in teal. We also show curves for the escape velocity of an NFW profile for the median mass of our sample. The gray bands show the same curve for the 16th and 84th mass percentile in the CUBS-Dwarfs sample. (Bottom) The radial velocity of absorbers, normalized by the estimated escape velocity of associated galaxy halos. The dotted lines represent the border between the formally bound and unbound absorbers. Approximately 15% of the dwarf galaxies exhibit formally unbound metal absorption.
Paper: The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O VI Absorption
Authors: Nishant Mishra, Sean D. Johnson, Gwen C. Rudie, Hsiao-Wen Chen, Joop Schaye, Zhijie Qu, Fakhri S. Zahedy, Erin T. Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Claude-André Faucher-Giguére, Jenny E. Greene, Jennifer I-Hsiu Li, Zhuoqi (Will) Liu, Sebastian Lopez, Patrick Petitjean
Figure caption: The stellar mass (﹩\mathrm{log}{M}_{\star }/{M}_{\odot }﹩), redshift (z), and virial radius normalized project distance (d proj/R vir) distributions of the sample plotted against each other with histograms plotted along the diagonal. The CUBS-Dwarfs sample is shown in circles and solid lines while the dwarf sample from S. D. Johnson et al. (2017) is shown with orange square symbols and dotted lines for comparison. The 91 CUBS-Dwarfs galaxies enable studies of the multiphase CGM/IGM around dwarf galaxies with a ninefold increase in sample size, including an emphasis on d proj/R vir > 1 and z > 0.3.
Paper: Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Authors: Ekta Patel, Lipika Chatur, Yao-Yuan Mao
Figure caption: Top left: the cumulative number of satellite galaxies as a function of 3D distance relative to the MW at the present day (solid blue), 1 Gyr ago (dashed orange), and 2 Gyr ago (dotted green) from orbits calculated in a joint MW+LMC potential. Shaded regions correspond to the 68% confidence intervals on the radial distribution at each time. Colored vertical lines illustrate the R 50 value for each data set, the radius at which half of the satellites are encompassed. The black vertical line shows the present-day location of the LMC. The legend indicates how many satellites are included at each time step. We do not correct for completeness. Bottom left: the difference between pairs of radial distributions as a function of 3D distance. The black line shows the difference between the present-day and 1 Gyr ago radial profiles, while the gray line indicates the difference between the 1 and 2 Gyr ago distributions. Radial profiles are less concentrated at previous epochs than today. The largest differences in radial profiles between the present day and 1 Gyr ago are in the innermost regions (D < 150 kpc), while the difference between the radial profiles 1 and 2 Gyr ago is more apparent in the outer regions (D > 150 kpc). Top right: same as the left panel, but the gravitational influence of the LMC has been removed, as well as the LMC plus four satellites within R vir of the LMC at infall (2.2 Gyr ago) and today. These satellites include the SMC, Carina III, Phoenix II, and Sculptor. Bottom right: the difference between radial distributions for the present day and 1 Gyr ago (black) and 1 Gyr ago and 2 Gyr ago (gray). The radial distributions evolve minimally compared to the left panel, implying that the presence of the LMC and its satellites drives the redistribution of satellites over time.
Paper: Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Authors: Ekta Patel, Lipika Chatur, Yao-Yuan Mao
Figure caption: Left: the cumulative radial profile for satellites with M  V  < −11.9 mag at D < 300 kpc in the joint MW+LMC potential. This magnitude selection reduces the MW sample to only four or five satellites, as indicated in the legend. Right: the distribution of R 50, the radius encompassing half of the satellites within 300 kpc of the MW, at the present day (blue histogram), 1 Gyr ago (orange histogram), and 2 Gyr ago (green histogram) for satellites with M  V  < −11.9 mag. The thick black line represents the average R 50 for the 101 hosts included in Data Release 3 (DR3) of the SAGA survey (Y.-Y. Mao et al. 2024). The thin, dashed black line represents R 50 for the subset of the 25% most concentrated SAGA DR3 hosts. The thick gray line illustrates the average R 50 from a sample of hosts included in the ELVES survey (S. G. Carlsten et al. 2022). The MW’s present-day R 50 is most consistent with the highly concentrated hosts in SAGA DR3, while the average SAGA DR3 and ELVES R 50 values are significantly larger than the MW population even at 1–2 Gyr ago.
Paper: Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies
Authors: Ekta Patel, Lipika Chatur, Yao-Yuan Mao
Figure caption: The evolution of R 50 with time for all satellites in the Rigid MW+LMC potential (dashed magenta line), all satellites in the Rigid MW potential (dotted black line), and satellites in the Rigid MW potential excluding the LMC and its satellites (solid black line). Lines track the median of R 50 across 1000 radial profiles constructed at each time step. Error bars represent the 25th and 75th percentiles of R 50.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Host-galaxy spectrum extracted from the last KCWI observations. The small right panels shows insets around [N II] λ6584 (top, marginally detected) and [O I] λ6300 (undetected).
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Preexplosion survey photometry from ZTF and ATLAS showing no outbursts or variability in the 8 yr preceding explosion. Single-night photometry is shown as small points with gray uncertainties whereas 30 day binned photometry is represented with larger bold points. Marker colors and symbols are the same as Figure 2.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Early light curve of SN 2023ufx showing the adopted time of explosion (﹩{t}_{\exp }﹩) marked with a downwards arrow. Only g-band and o-band light curves are shown for clarity. Open symbols are synthesized from the first SNIFS spectrum.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Comparing the g-band light curve of SN 2023ufx (black) to the sample from S. Valenti et al. (2016). We show the absolute magnitudes (top) and the magnitudes relative to peak (bottom) color coded according to peak absolute magnitude.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: The velocity anisotropy for halo stars, reported as a function of the galactocentric radius, r, divided by the NFW scale radius, r  s . We first calculate the velocity anisotropy profiles for particles in each individual galaxy system, with each curve referring to the median of a population of galaxies in the same bin of M 200. The legend shows the corresponding range in ﹩{\mathrm{log}}_{10}{{M}}_{200}/{{M}}_{\odot }﹩. The error bars are the 1σ scatters of 100 bootstrapped subsamples of galaxies in the same mass bin.