adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: The evolution of density contrast of three halo samples with different mass. The solid and dashed lines correspond to ﹩{\rm{\Delta }}\left(\lt {r}_{\mathrm{id}}\right)﹩ and ﹩{\rm{\Delta }}\left(\lt {r}_{\mathrm{cd}}\right)﹩, respectively. Different colors represent different mass. The dotted gray line represents ﹩0.18\times {\rm{\Delta }}\left(\lt {r}_{\mathrm{vir}}\right)﹩.
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: Evolution of the power-law slopes measured from the scaled enclosed mass profiles (Figure 4) between r vir and r id. The blue and red colors correspond to the galactic halo and the cluster halo sample, respectively.
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: Similar to Figure 3, but using the original FOF halo catalog before cleaning. Note that the determination of r id, and hence Δ(<r id), can be problematic for galactic halos at low redshifts.
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: Evolution of the scaled enclosed mass profiles. Each profile has been scaled by the virial radius r vir and the virial mass M vir. The inner depletion radii r id are also marked with a cross on each profile.
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: Similar to Figure 2, but using the original FOF halo catalog before cleaning. Note that the determination of r id can be problematic for galactic halos at low redshifts.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Matrix of plots showing the median fitted values vs. the true values from synthetic galaxy fits. The values are standardized using the sample mean and standard deviation so that the scatter in stellar mass can be compared to the slope and bump strength scatter. Shown are the parameters stellar mass, δ, and E  b  for each of the SFH assumptions. We find that the exponential SFH, while being the simplest model, did not lead to the most precise parameter recovery for stellar mass, δ, or E  b . Additionally, the most complex SFH, the piecewise, had the smallest scatter in recovering δ.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Comparison of dust law parameters when fit with and without UVOT data. Left: the attenuation law slope with UVOT vs. the slope when fit without UVOT. Right: the 2175 Å bump strength with UVOT vs. the bump from fits without UVOT data. We see that there is fairly good agreement on the slope of the attenuation law between fits with and without UVOT data. However, there is a noticeable difference when including the UVOT data for the bump strength. We find that fits with the UVOT data lead to bump strengths that are ∼2/3 to 3/4 of the bump as determined without UVOT photometry. This could point toward the inability to measure the bump strength accurately without additional NUV data. Characteristic errors are shown in the upper left of each plot. We see that including UVOT leads to a reduction in the size of the error bars.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Average attenuation curves for the SINGS/KINGFISH sample. Left: mean attenuation law of the entire sample, calculated by averaging over the entire sample at each wavelength for each different SFH tested. Right: mean attenuation law from the piecewise SFH fits compared to the starburst law, excluding galaxies consistent with no dust. The 16th and 84th percentiles are shown for the piecewise SFH result and the Calzetti et al. (2000) error in R  V  is displayed. We see that the derived attenuation law for each SFH is steeper than the Calzetti et al. (2000) law.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Density plots in the δ–E  b  plane for the fits using the double-power-law SFH. The values from fits including UVOT data are in line with the expectation from Kriek & Conroy (2013), while the fits without lie systematically above. The black dashed line shows the median of the uniform bound prior. The bump strengths from the fits without UVOT data are clustered around that point, implying that the fits without UVOT data cannot constrain the bump beyond the uninformative prior.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Sample average attenuation law compared from fits with and without UVOT photometry. We find that the average bump strength is smaller when including the UVOT data. We also see a small shift to shallower slopes. This means that when determining the attenuation curve without UVOT data, it is likely that one will overestimate the amount of attenuation at all wavelengths. This is compared to the starburst law, which significantly underestimates attenuation, regardless of photometry used and the SFH parameterization assumed.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Matrix of plots showing median fitted vs. true values for fits to mock galaxies, done without UVOT data. As in Figure 9, we are plotting the values standardized by the sample mean and standard deviation. We find confirmation that the additional data increase precision in recovering the dust law parameters. Contrasting with the fits of real data, we do not see a shift in bump strength when removing the UVOT data. The different result seen based on fits to real vs. synthetic photometry warrants further discussion and investigation.
Paper: No Small-scale Radio Jets Here: Multiepoch Observations of Radio Continuum Structures in NGC 1068 with the VLBA
Authors: Travis C. Fischer, Megan C. Johnson, Nathan J. Secrest, D. Michael Crenshaw, Steven B. Kraemer
Figure caption: Multiband imaging of the nuclear region of NGC 1068, centered on the approximate location of the AGN. First row: continuum-subtracted ALMA Band 7 observations of CO(3-2) 345.796 GHz emission with contoured comparisons of [Fe II] 1.644 μm (second column; red), [O III] λ5007 (third column; green), and 8.49 GHz radio continuum (fourth column; blue) features. Second row: continuum-subtracted Gemini NIFS IFU imaging of [Fe II] 1.644 μm emission with contoured comparisons of [O III] λ5007 (second column; green), and 8.49 GHz radio continuum (third column; blue) features. Third row: continuum-subtracted HST WFPC2 imaging of [O III] λ5007 emission with a comparison to 8.49 GHz radio continuum (second column; blue). Bottom row: VLA A-Array imaging of 8.49 GHz radio continuum. Outer contours of [Fe II], [O III], and radio continuum imaging represent signal-to-noise ratios of 12σ, 100σ, and 10σ, respectively. North is up and east is to the left.
Paper: No Small-scale Radio Jets Here: Multiepoch Observations of Radio Continuum Structures in NGC 1068 with the VLBA
Authors: Travis C. Fischer, Megan C. Johnson, Nathan J. Secrest, D. Michael Crenshaw, Steven B. Kraemer
Figure caption: Left: composite image showing the central region of NGC 1068 where red is HST broadband WFPC2 filter F547M, green is the continuum-subtracted HST [O III], and blue is the VLA A-array 5 GHz continuum map. Right: composite image showing the VLBA 6 GHz radio continuum data from Fischer et al. (2021) for NGC 1068 (yellow) with VLBA 5 GHz radio continuum data from Gallimore et al. (2004) (cyan).
Paper: No Small-scale Radio Jets Here: Multiepoch Observations of Radio Continuum Structures in NGC 1068 with the VLBA
Authors: Travis C. Fischer, Megan C. Johnson, Nathan J. Secrest, D. Michael Crenshaw, Steven B. Kraemer
Figure caption: Epoch 2 VLBA 6 GHz radio continuum data with archival VLA A-array 8.49 GHz continuum imaging contours (green) overlaid. Knots NE and C in Epoch 2 are circled in white with arrows pointing in the direction of their measured velocity vectors (not to scale). The central active galactic nucleus (AGN) is circled in yellow. Cyan, dashed lines point to the apex positions of the extended radio sources shown in Figure 1. The kinematic major axis of the rotating molecular gas, per García-Burillo et al. (2019), is shown as blue and red lines, with rotation traveling counterclockwise on the plane of the sky.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Distributions of SDSS galaxies on the SFR–mass diagram. The left and right panels show the distribution of early- and late-type galaxies, respectively. Only 2% of the data are shown in the diagram for clarity. The red and blue circles represent 20% of galaxies with IFS data from the MaNGA survey. The thick solid line on the diagram represents the star-forming main sequence (Elbaz et al. 2007) and the dashed line represents a factor of 4 below the star-forming main sequence. We classify galaxies into star-forming and quiescent galaxies by the criterion of the dashed line.
Paper: No Small-scale Radio Jets Here: Multiepoch Observations of Radio Continuum Structures in NGC 1068 with the VLBA
Authors: Travis C. Fischer, Megan C. Johnson, Nathan J. Secrest, D. Michael Crenshaw, Steven B. Kraemer
Figure caption: Locations of Gaia EDR3 astrometric reference points used to correct the HST astrometry, overlaid on the F547M image used for the counterparts.
Paper: Constraining the Evolution of the Unstable Accretion Disk in SMC X-1 with NICER
Authors: McKinley C. Brumback, Georgios Vasilopoulos, Joel B. Coley, Kristen Dage, Jon M. Miller
Figure caption: Phase-averaged spectra for Observation 307 (left) and Observation 402 (right) with the best-fit spectral model tbabs ∗ (cutoffpl+blackbody+apec+gaus) (top residual panel). The bottom two residual panels show alternative model components. The middle residual panels show the use of pow instead of cutoffpl, which fails to accurately describe the power-law tail in all spectra. The bottom residual panels show the best-fit model without apec, the strength of which varies strongly between observations. This effect is illustrated here by the significant low-energy residuals in Observation 402 (demonstrating a strong requirement for apec) compared to the minimal change in residuals in Observation 307. However, even in the case of Observation 307 the data prefer the presence of apec, with a Δχ 2 of 8.6.
Paper: Constraining the Evolution of the Unstable Accretion Disk in SMC X-1 with NICER
Authors: McKinley C. Brumback, Georgios Vasilopoulos, Joel B. Coley, Kristen Dage, Jon M. Miller
Figure caption: Pulse phase-resolved spectral parameters for Observations 307 and 402 as an example of the behavior seen in the full data set. In all panels, the solid black line is the full-bandpass NICER pulse profile. Both the pulse profile and the parameter values have been normalized against their mean values to enable plotting on a uniform scale. First panel (blue squares): the photon index shows strong variation with pulse phase, increasing in strength during the pulse trough and decreasing during the pulse peak. Second panel (purple triangles): the N H does not show changes with pulse phase in some observations, like 307, while in others it does show changes, as in Observation 402. Third panel (navy circles): the normalization of the blackbody component follows the shape of the pulse profile. Fourth panel (red squares): the normalization of the power-law component follows the shape of the pulse profile.
Paper: Constraining the Evolution of the Unstable Accretion Disk in SMC X-1 with NICER
Authors: McKinley C. Brumback, Georgios Vasilopoulos, Joel B. Coley, Kristen Dage, Jon M. Miller
Figure caption: The key phase-averaged spectral parameters for our data set as a function of time. Panel (A) (gray points): the Swift/BAT 15–50 keV light curve for SMC X-1. Panel (B) (purple triangles): the absorbing column density (N H). Panel (C) (navy circles): the blackbody temperature. Only one point for each epoch, corresponding to the brightest observation, shows the error bars; in the other observations, the temperature is fixed to the value from the brightest observation. Panel (D) (blue squares): the photon index. Panel (E) (light blue triangles): the plasma temperature from apec. Epochs 1 and 2, which occur during the intermediate state of the superorbital cycle, show the most significant differences in spectral parameters between cycles. Epochs 3 and 4 have values more consistent with each other.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Distribution of Type Iax SNe in terms of the peak absolute magnitude and rise time in r/R-band. The figure clearly depicts the fact that Type Iax SNe follow a correlation in their peak luminosity and rise time.
Paper: Constraining the Evolution of the Unstable Accretion Disk in SMC X-1 with NICER
Authors: McKinley C. Brumback, Georgios Vasilopoulos, Joel B. Coley, Kristen Dage, Jon M. Miller
Figure caption: Pulse profiles for our data set in the full NICER bandpass. Pulse profiles have been shifted to align the primary pulse peak and all plotted with the same y-axis scale. All profiles show the double-peaked structure characteristic of SMC X-1, but the relative strength of the pulse peaks varies between observations.
Paper: Constraining the Evolution of the Unstable Accretion Disk in SMC X-1 with NICER
Authors: McKinley C. Brumback, Georgios Vasilopoulos, Joel B. Coley, Kristen Dage, Jon M. Miller
Figure caption: The Swift/BAT 15–50 keV light curve for SMC X-1 (black) showing the superorbital modulation around the time of our NICER observations (blue dashed lines). The observations occurred during the bright high state of four superorbital cycles, referred to in this work as Epoch 1–4. Epoch 1 contains five NICER visits, Epoch 2 contains four NICER visits, Epoch 2 contains seven NICER visits, and Epoch 4 contains two NICER visits for a total of 18 observations.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Absolute magnitude vs. light-curve decline rate in r/R-band for well-studied Type Iax SNe.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Same as in Figure 15 but for SN 2020kyg.
Paper: O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy
Authors: Kotaro Fukushima, Shogo B. Kobayashi, Kyoko Matsushita
Figure caption: The Fe and O abundances and the Ne/O, Mg/O, O/Fe, Ne/Fe, and Ni/Fe ratios as functions of 〈kT〉 (left column) and M <60″/L  B  (right column). The filled and open circles represent the results with AtomDB and SPEXACT, respectively. The stars indicate the results for Centaurus (Fukushima et al. 2022a). Errors are shown only for the AtomDB results for viewing purposes. We also show ratios expected by two major CCSN nucleosynthesis models (Nomoto et al. 2006; Sukhbold et al. 2016) on the Ne/O and Mg/O panels. The Pearson’s correlation coefficients with the AtomDB results are shown in the top right corner of each panel.
Paper: O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy
Authors: Kotaro Fukushima, Shogo B. Kobayashi, Kyoko Matsushita
Figure caption: Abundance ratio patterns obtained in central 60″ cores. The sample is divided into two subsamples using temperature regimes (circles) and M <60″/L  B  = 0.1 M ⊙/L ⊙ (ties), for each of which the abundance ratios are averaged. The stars represent the result for the Centaurus cluster given in Fukushima et al. (2022a). Filled and open symbols indicate the results of AtomDB and SPEXACT, respectively. To fit the observed pattern, we adopt two combination models of CCSN and SN Ia yields: the “classical” CCSN model (Nomoto et al. 2006) and W7 model (Iwamoto et al. 1999), and the N20 model (Sukhbold et al. 2016) and new W7 model (Leung & Nomoto 2018). Every progenitor metallicity thereof is assumed to be 1 solar. For viewing purposes, only two combinations with the best χ 2/dof are presented for M <60″/L  B  subsamples with AtomDB. See Table 5 for the results of other regimes and the other combination.
Paper: O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy
Authors: Kotaro Fukushima, Shogo B. Kobayashi, Kyoko Matsushita
Figure caption: The N/O ratios as functions of (a) 〈kT〉 and (b) M <60″/L  B . The filled and open circles represent the results with AtomDB and SPEXACT, respectively. The stars indicate the results for Centaurus (Fukushima et al. 2022a). Errors are shown only for the AtomDB results for viewing purposes. The ratios predicted by Karakas (2010) are shown by horizontal solid lines, assuming the initial metallicity of AGB stars at each mass to be the solar value. The Pearson’s correlation coefficients for the AtomDB results are given in the top right corner of each panel.
Paper: O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy
Authors: Kotaro Fukushima, Shogo B. Kobayashi, Kyoko Matsushita
Figure caption: XRISM simulated spectrum of the central arcminute of NGC 4649. The current RGS data within the 60″ region are also plotted in dark cyan. The red and dark blue lines represent the best-fit models without Ne and Ni lines, respectively. Prominent emission lines are marked on the upper panel.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Normalized polarization measurements of the outflow as a function of the normalized vertical height. The normalized total flux (left-hand), polarized flux (middle), and integrated polarization fraction (right-hand) are shown as a function of the normalized vertical height at the peak of the total flux, ﹩h/{h}_{\mathrm{peak}}^{I}﹩, polarized flux, ﹩h/{h}_{\mathrm{peak}}^{{PI}}﹩, and integrated polarization fraction, ﹩h/{h}_{\mathrm{peak}}^{{P}^{\mathrm{int}}}﹩. The vertical heights at the peak of the polarized flux and integrated polarization fraction are shown in Appendix B (Table 4). The linewidths increase with the wavelength for each galaxy, as shown in the top legend. Several power laws as indicated in each panel are shown.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Polarization measurements as a function of the vertical height across the outflow. Top: the total flux (left-hand, polarized flux (middle), and polarization fraction (right-hand) as a function of the vertical height. The linewidths increase with the wavelength for each galaxy, as shown in the top legend. Bottom: the SEDs of the total flux (left-hand), polarized flux (middle), and polarization fraction (right-hand). The color scale changes with the vertical height, as shown in the color bar. The marker size increases with the polarization fraction, as shown in the bottom left-hand legend.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: The polarization spectra of starburst galaxies. The integrated polarization spectra (P int;  top) for the full galaxy (left-hand), disk (middle), and outflow (right-hand) of M 82 (orange), NGC 253 (green), and NGC 2146 (gray) are shown. The normalized polarization spectra (﹩{P}^{\mathrm{int}}/{P}_{154\,\mu {\rm{m}}}^{\mathrm{int}};﹩ bottom) for the same regions and galaxies are shown.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: In search of the B-field signature along the galactic outflows of starburst galaxies: M 82 as the case study. Optical polarimetric observations are dominated by dust scattering (left-hand panel) (Neininger et al. 1990; Fendt et al. 1998). The lines show the E-vectors with the 10% polarization legend shown in the bottom left-hand corner. FIR polarimetry observations reliably trace the B-fields in the galactic outflows (middle panel) (Jones et al. 2019; Lopez-Rodriguez et al. 2021; Borlaff et al. 2023). Radio polarimetric observations have short lifetime cosmic rays along the galactic outflow and only a magnetized bar is measured (right-hand panel) (e.g., Thompson et al. 2006; Adebahr et al. 2017). For both FIR and radio, the lines show the B-field orientation with constant length.