adsabs/AstroCLIMB huggingface dataset:
Paper: Distance Duality Test: The Evolution of Radio Sources Mimics a Nonexpanding Universe
Authors: Pengfei Li
Figure caption: The distance duality relation for the combined sample from Jackson & Jannetta (2006) and Gurvits et al. (1999). The total 943 radio sources are distributed into 27 bins. The median values of D  L (z)/D  A (z) within each bin are plotted against redshift. The predictions of the nonexpanding and expanding universes are presented as the solid and dashed lines, respectively. The data show a linear distance duality relation, consistent with Euclidean geometry.
Paper: Distance Duality Test: The Evolution of Radio Sources Mimics a Nonexpanding Universe
Authors: Pengfei Li
Figure caption: The systematic dependence of radio luminosity on redshift for 613 radio sources at 2.29 GHz (left) from Jackson & Jannetta (2006) and 330 sources at 5.0 GHz (right) from Gurvits et al. (1999). The solid lines are the best-fit relations in the given parameterization form.
Paper: Distance Duality Test: The Evolution of Radio Sources Mimics a Nonexpanding Universe
Authors: Pengfei Li
Figure caption: The histogram of spectral index (S ∝ ν  α ) for 572 radio sources at 2.29 GHz compiled in Jackson & Jannetta (2006). The values of α are picked from Preston et al. (1985).
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: (Top) Plots of [C/Fe] ch  and [N/Fe] nh  of individual M22 RGB stars against V magnitude. The blue and red colors denote the MP and MR populations. The error bars in (a) and (b) are for typical measurement uncertainties in our [C/Fe] ch  and [N/Fe] nh  derivation, respectively. (Bottom) Same as the top panels but the results from the dereddened color indices.
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: (a) The [Fe/H] hk  distribution of M22 RGB stars. The blue and red colors denote the MP and MR populations. (b) The histogram of the [Fe/H] hk  along with results returned from our EM estimator. (c) CRDs of each RGB population. (d)–(f) Same as (a)–(c) but for the [Fe/H] hk  from the dereddened hk JWL colors.
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: CMDs of member RGB stars with −2.5 mag ≤ V − V HB ≤ 3.0 mag in M22. In the top panels, we show differential reddening vectors of individual color indices for ΔE(B − V) = 0.1 mag with red arrows.
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: (Top) CMDs of M22 in our science field. (Bottom) CMDs for M22 proper-motion member stars.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: In the left column, the in situ profiles of the magnitude of the magnetic field for both events are plotted in black in panels (a) and (b), respectively. The background in green signifies the flux rope region that shows a drop in plasma β value. We consider a tapered flux rope model to develop the 3D structure of the ICMEs, as shown in the red lines. The dashed blue lines in both panels depict the associated axially symmetric flux rope near Earth without any interaction during the heliospheric propagation of the CME. In reality, some part of that symmetric flux rope (the leading edge for event 1 in panel (a) and the trailing edge for event 2 in panel (b)) vanishes due to possible interactions with the interplanetary medium before reaching Earth. The remaining modeled flux rope is shown using the red line within the green patched region. In panel (c), we plot a cartoon of an axisymmetric flux rope (in blue) and a tapered flux rope (in maroon) side by side for an overall understanding. The tapered flux rope has an eroded edge due to interplanetary interactions. The radius of the axisymmetric flux rope is taken to be the same as the length between the core and the distant boundary of the tapered flux rope (marked with arrows).
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: Comparison between the ICME structure embedded in the solar wind (black lines) and the modeled input (red lines) in the GSE coordinate system for event 1 in (a) and event 2 in (b), respectively. The initial dotted red line in the modeled profiles corresponds to the solar wind input that forced the magnetosphere to a steady state. The interplanetary conditions are plotted using the Wind Magnetic Field Investigation (MFI) data provided by the NASA Coordinated Data Analysis Web (CDAWeb) service. The modeled profile is measured at a single point on the x-line at the dayside domain boundary and then time-shifted to the average x-position of the Wind spacecraft, which was at the nightside of Earth (∼  −213 R E) for event 1 and at dayside (∼199 R E) for event 2.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: The top panels (a)–(j) show side-by-side comparisons of modeled magnetic field profiles (left column) and corresponding STORMI (storm intensity) index profiles (right column) for different erosion scenarios. The standard deviations for the estimates are encapsulated in the width of the STORMI index curves. Each row represents a different case, which is noted in the plots. The black dashed lines in the plots on the left column are fits assuming an underlying axisymmetric profile; these indicate departures from an axisymmetric flux rope (as in Figure 5). Timestamp is maintained at Earth’s location to account for propagation delays. The bottom image (panel (k)) displays a superimposed plot of the STORMI index for all cases. The maximum change in the index due to tapering is approximately 9 nT, which is in the leading-edge regions, while in the trailing-edge regions, it is less than 3 nT. However, these changes are localized near the flux rope boundary for individual cases and do not significantly impact the overall storm intensity profiles or the maximal impact.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: Simulated 3D view of the planetary magnetosphere from a viewpoint just above the ecliptic plane. The magnetospheric fields are depicted using colored lines to distinguish among the Earth’s polar open field lines (orange), the closed inner magnetospheric lines (cyan), and IMF (green). The strong event (event 1) that occurred on 2003 November 20 is shown in panel (a), and the moderate event (event 2) of 2006 April 14 is shown in panel (b). The white arrows in both images denote the rotation axis of Earth. The magnitude of the current density (J) is plotted on the equatorial planes to demonstrate the current formation around the Earth right after the passage of the leading halves of the flux ropes for event 1 (top) and event 2 (bottom). The yellow arrows designate the Sun-side (along the x-axis).
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: Cross-sectional θ-shaped current systems of the magnetotail for event 1 (top row) and event 2 (bottom row). The current density (J) is plotted in the YZ plane (STORMI’s coordinate system) at a distance of 60R  E  from Earth and is viewed from the magnetotail side. Panels (a) and (g) shows the current boundaries of the magnetotail due to solar wind forcing before the ICME’s arrival. In the second column, (b) and (h) reveal the magnetotail currents during the ICME sheath for events 1 and 2, respectively. Panels (c) and (i) show the current system during initial ICME forcing for the events. For the rest of event 1, the magnetotail gets stretched maximally along the semimajor axis as depicted in (d) and starts decreasing in (e) as the trailing part of the ICME crosses the Earth. In (f) the solar wind forcing reshapes the magnetotail away from the perturbed state. On the other hand, (j) and (k) shows the simulated magnetotail during the maximum impact during the transit of the trailing part of the ICME for event 2. Panel (l) shows the post-ICME solar wind-forced magnetotail.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: The figure presents the comparison of the time evolution of the Dst index (black dashed curve), SYM-H index (solid black line), and the modeled reduction in the geomagnetic field intensity in terms of STORMI index (blue curve) for event 1 in panel (a) and for event 2 in panel (b). The semitransparent blue-shaded region is the standard deviation of the STORMI geomagnetic storm index. The STORMI index is computed after incorporating the time delay between the in situ observations of the solar wind (shown in Figure 1) and its geomagnetic perturbation.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: Panel (a) and (b) depicts the distribution of time-averaged quiet-time current density, surface-averaged over planes parallel to the equatorial plane for event 1 and event 2, respectively, as a function of the height from the equator. The center of the horizontal axis denotes the equator with zero height. A positive height represents a plane in the northern hemisphere, and a negative height indicates a plane in the southern hemisphere. The vertical black lines mark the height of the plane that has a local minimum value of average current near the equator.
Paper: A Time-efficient, Data-driven Modeling Approach for Predicting the Geomagnetic Impact of Coronal Mass Ejections
Authors: Souvik Roy, Dibyendu Nandy
Figure caption: The figure shows the 3D distribution of the 12 points around the equator marked as blue squares. The equator is projected to the XY plane in STORMI’s coordinate system. The points are chosen as the nearest grid centers placed just outside the black circle with a radius equal to Earth’s. The background cells correspond to the near-Earth grid resolution of STORMI, where each corner represents a grid center.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: Radius vs. effective Temperature and metallicity fits of stars within 4.″2 of the hydrodynamic center of SNR 0509−67.5, the sample of potential surviving companion stars. The gray crosses show the surrounding control sample from Figure 4 that we used to estimate the underlying temperature-radius distribution of the local stellar population, shown by the contours. The purple crosses show the three stars identified in A22. The red x markers show surviving companion models from Table 2 close enough to be compared, with the other models too high in temperature or large in radius to be placed within the bounds of the figure.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: Radius vs. effective Temperature and metallicity fits of stars in a 10″ radius, excluding those close enough to the center of SNR 0509−67.5 to be the surviving companion. We used this sample to estimate the underlying main sequence distribution of stars in the local LMC. We note the presence of two anomalous large radius stars that we do not support belonging to the local main sequence population and thus do not include in our distribution estimation in Figure 5. We discuss these stars further in Section 4.2.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: An example showing the effects of metallicity at different temperatures. The top panel shows the spectra of a metal-poor (﹩[\tfrac{M}{H}]=-1﹩) 6000 K star and a metal-rich (﹩[\tfrac{M}{H}]=1﹩) 6000 K star. The bottom shows the same but comparing 10,000 K stars. The purple dashed lines show the transmission curves of the same filters used in the rest of this work, and the gray line shows the difference between the two spectra. At some temperatures, sufficiently sensitive photometry is capable of constraining metallicity, detecting relative enhancements and diminishments in the redder and bluer optical portions of the spectrum.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: An example outcome of the fitting process for one of the stars in the search region. The blue crosses show the photometric observations with the vertical spread showing observational uncertainty, and the horizontal spread shows the width of the filter used for the observation, corresponding to the rough portion of the spectrum probed by the observation. The transmission curve of each filter is shown in dashed purple. The black and gray regions show a distribution of spectra created by sampling the posterior distribution of constrained stellar parameters.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: A composite image of SNR 0509−67.5 from archival photometry. The red channel is the F814W filter, green is F555W, and blue is F656N. The red circle shows our search region where stars are close enough to the center to be the surviving companion, and the green region shows the larger control sample of characterized stars we used to better understand the unrelated stellar population and the uncertainties of our technique. The white circles show the individual stars that were modeled and characterized. The two large stars we discuss in Section 4.2 are circled in pink.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: An example fit corner plot of extracted astrophysical parameters of the Sun for methodological validation. We obtained and fit magnitudes from Willmer (2018). The true values are shown with blue lines. Our parameter extraction shows strong agreement with the true solar values of temperature and radius, within 1σ.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: Our fit for HHE 5, similar to that shown in Figure 3. The model does a poor job fitting the observations, primarily because of the single F814W observation that is impossible to explain with a stellar spectrum capable of fitting the other four observations. The other points can be suitably explained by a typical stellar spectrum, in accordance with the possibility of an unphysical F814W measurement.
Paper: No Surviving SN Ia Companion in SNR 0509-67.5: Stellar Population Characterization and Comparison to Models
Authors: Joshua V. Shields, Prasiddha Arunachalam, Wolfgang Kerzendorf, John P. Hughes, Sofia Biriouk, Hayden Monk, Johannes Buchner
Figure caption: Error on magnitude as a function of magnitude for the full set of characterized stars in the larger sample, by filter. These data show the observational uncertainties used for our Bayesian inference fitting.
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: Plots of [C/Fe] ch  vs. M  V  of individual populations of M22, M5, M3, and M92 for RGB stars brighter than their RGBB V magnitudes. The blue and red solid lines denote the least-squares fitting and the robust fitting by minimizing absolute deviation, respectively. The numbers in parentheses are the mean metallicity of each GC.
Paper: Carbon Abundance of Globular Cluster M22 (NGC 6656) and the Surface Carbon Depletion Rates of the Milky Way Globular Clusters
Authors: Jae-Woo Lee
Figure caption: (a) A plot of d[C/Fe]/M  V  vs. [Fe/H] returned from the least-squares fitting (blue solid lines in Figure 5). The blue and red colors denote the FG and SG, respectively. The green and gold solid lines show a linear regression with confidence intervals of 95%. The yellow shade box indicates the mean value by Smith & Martell (2003). (b) Same as (a) but for results returned from the robust fitting by minimizing absolute deviation (red solid lines in Figure 5).
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Median rest-frame SEDs of SF (left), mixed (middle), and AGN (right) types. The red curves indicate the median SEDs. The gray curves indicate the MIRI SEDs (only S/N > 3 MIRI points are being used here for high quality) for individual sources. All these individual SEDs are normalized at rest-frame 3.6 μm. The median SEDs are estimated from these gray curves. In the left panel, we also display two local-SF galaxy SEDs, NGC 5992 and NGC 6090, from Brown et al. (2014). Our median SF SED is similar to the SEDs of these two local-SF galaxies. In the right panel, we also display the median SED for hot dust-obscured galaxies (hot DOG; Fan et al. 2016) and the average SED for the nuclear regions of Seyfert 2 galaxies (Videla et al. 2013). These typical SEDs are similar to our MIRI-selected AGN median SED.
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Black hole accretion density as a function of redshift. The red data points are derived based on our MIRI-selected AGN; the orange ones are from AGN+mixed sources. The vertical error bars consider both bootstrap and SED-fit (Bayesian) uncertainties; the horizontal error bars indicate the redshift bins. The orange curve representing the inferred BHAR for bulge-dominated galaxies is from Yang et al. (2021a), and is thereby a lower bound on the total accretion rate. The black curves are from X-ray measurements with references marked in the legend (see Yang et al. 2021a for details). At high redshifts of z ≳ 3, our MIRI-based BHAD values are significantly higher than the corresponding X-ray measurements, but are consistent with the Yang et al. (2021a) lower bound. The blue curve represents SFRD (Madau & Dickinson 2014) downscaled by a factor of 2000 to roughly match the X-ray-based BHAD peak at z ∼ 2.
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption:  L disk distributions for AGN (red, with fracAGN ≥ 0.5) and mixed (blue, with 0.1 < fracAGN < 0.5) objects. Different panels are from different redshift bins as labeled. The vertical dashed lines indicate the typical knee luminosities from Shen et al. (2020). The corresponding BHAR is also marked at the upper axis. L disk is numerically equivalent to angle-averaged L bol (see Section 3.2).
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Comparison between different types of rest-frame median SEDs (same as in Figure 4). The blue, orange, and red represent SF, mixed, and AGN types, respectively. The shaded regions indicate the corresponding 1σ scatters, estimated as 16th–84th percentiles. The AGN SED is distinctive from the SF SED. These median SEDs and their associated errors are publicly available with this figure.(The data used to create this figure are available.)
Paper: CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts
Authors: G. Yang, 光 杨, K. I. Caputi, C. Papovich, P. Arrabal Haro, M. B. Bagley, P. Behroozi, E. F. Bell, L. Bisigello, V. Buat, D. Burgarella, Y. Cheng, N. J. Cleri, R. Davé, M. Dickinson, D. Elbaz, H. C. Ferguson, S. L. Finkelstein, N. A. Grogin, N. P. Hathi, M. Hirschmann, B. W. Holwerda, M. Huertas-Company, T. A. Hutchison, E. Iani, J. S. Kartaltepe, A. Kirkpatrick, D. D. Kocevski, A. M. Koekemoer, V. Kokorev, R. L. Larson, R. A. Lucas, P. G. Pérez-González, P. Rinaldi, L. Shen, J. R. Trump, A. de la Vega, L. Y. A. Yung, J. A. Zavala
Figure caption: Top: comparison between our photometric redshifts (from CIGALE fits) vs. spectroscopic redshifts (when available). The red solid line indicates the 1:1 relation, while the red dashed lines indicate a 15% uncertainty (beyond which a source would be considered as a photo-z outlier). The photo-z quality, quantified by σ NMAD and fracout, is marked. We note that the outlier fraction is zero. Bottom: relative difference between photo-z and spec-z as a function of H-band magnitude. Each red star represents the median value for each magnitude bin, while the horizontal error bar indicates the bin coverage. It appears the photo-z quality does not significantly depend on the magnitude.