adsabs/AstroCLIMB huggingface dataset:
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: The measured DESI LRG projected two-point autocorrelation in our three HSC–DESI overlap fields for our z ∈ 0.5–1.0 redshift bin. The open symbols are the per-bin inverse-variance-weighted average correlation function across fields. The 1σ uncertainties are drawn from the square root of the diagonal of the jackknife covariance matrix for the sample. The dashed lines represent the fitted DM halo model to each field. We fit points for physical scales rp > 1 h−1 Mpc, while the gray region contains the points at smaller scales excluded from the fit. Note that the model does not include the one-halo term, which is why the data rise significantly above the model on small scales.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Luminosity histograms for each of our AGN (sub)samples in the z ∈ 0.5–1.0 bin combining the three overlap fields in GAMA. The top and bottom panels show the original distributions, while the middle panel is normalized in order to show the consistency in the L6μm distribution between the complete, BL, and NL AGN samples. The vertical black dashed line is shared across the panels and denotes the L6μm = 3 × 1044 erg s−1 lower limit for this analysis.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Normalized spectroscopic redshift distribution of each AGN (sub)sample for the clustering analysis when combining the catalogs from all GAMA overlap fields, after applying redshift and L6μm thresholds. The black line is shared among all panels to compare with the complete AGN sample’s distribution.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Diagram visually describing our spectroscopic classification. See Section 4 for a detailed description of each of these steps.
Paper: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Authors: Jiayan Yang, Leping Li, Huadong Chen, Yi Bi, Bo Yang, Junchao Hong, Yan Dong
Figure caption: NLFFF extrapolation of the coronal magnetic topology and the decay index above the two filaments before ((a1)–(a3)) and after ((b1)–(b3)) F1’s eruption. The background image is the AIA 304 Å image captured at 01:44:53 UT. The overlying curves represent the extrapolated coronal magnetic field lines, among which the gray curves indicate the flux ropes of F1, the dark blue curves indicate the magnetic arcade above F2, and the cyan curves represent a common arcade covering both F1 and F2. The horizontal axes of panels (a3) and (b3) correspond to the spatial coordinate along the red line P1P2 in panel (a1). The white dotted lines in the bottom row indicate the height of the flux rope. The overlaid black lines on these lines correspond to the region shown by the blue segment of P1P2 in panel (a1).
Paper: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Authors: Jiayan Yang, Leping Li, Huadong Chen, Yi Bi, Bo Yang, Junchao Hong, Yan Dong
Figure caption: AIA 304, 171, 211, and 335 Å time–distance plots. The time-slices are constructed along the slit AB shown in Figure 2. The blue dotted lines in panel (b) mark the eruption of F1. The eruption and fall of F2 are visible in the right-hand side of all panels. The white arrows in panel (a) and the white dotted lines in panel (b) point out some traces of plasma flow following the eruption of F1. The dashed white line indicates the approximate time of F2’s eruption inferred from the time-slice of 211 Å images.
Paper: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Authors: Jiayan Yang, Leping Li, Huadong Chen, Yi Bi, Bo Yang, Junchao Hong, Yan Dong
Figure caption: AIA 304 Å ((a1)–(a2)), 171 Å ((c1)–(c2)), CHASE Hα ((b1)–(b2)) images and HMI LOS magnetograms ((d1)–(d2)) show the filaments and their surroundings prior to eruption. The white rectangles in the top row show the field of view (FOV) of the bottom row, while the white dotted curves indicate the trajectory of the following jet at 03:40:17 UT. The white arrows in panels (b1) and (b2) point to a quiescent filament QF and two filaments F1 and F2, while the blue and red curves in panel (d2) indicate the traced spines of F1 and F2 from panel (a2) by manual visual inspection. The white and blue contours superimposed on panels (a1), (a2), and (c2) represent the simultaneous HMI LOS magnetic field with intensities of ±150, ±400, and ±600 Gauss.
Paper: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Authors: Jiayan Yang, Leping Li, Huadong Chen, Yi Bi, Bo Yang, Junchao Hong, Yan Dong
Figure caption: ((a)–(b)) Time–distance plots along the jet spire in AIA 335 and 171 Å. (c) Time-space plot along a slit perpendicular to the jet spire in AIA 211 Å. The vertical white line indicates the start time of the jet. The two short white arrows point out the ejection and the descending phases of the jet respectively, and the dotted lines depict the linear fitting of the trajectory of these phases. The short black arrows show two episodes of the lateral motion of the jet. The positions of two slits S1 and S2 are indicated by blue arrows in Figure 5.
Paper: Sympathetic Eruption of Two Filaments and Associated Solar Coronal Jet
Authors: Jiayan Yang, Leping Li, Huadong Chen, Yi Bi, Bo Yang, Junchao Hong, Yan Dong
Figure caption: ((a1)–(b4)) Weak flares associated with eruptions of F1 and F2 showed in AIA 1600 Å and GONG Hα images. The axes of F1 and F2 obtained by manual visual inspection before the eruptions are superimposed as blue and red curves, respectively. The FOV is the same as in Figure 2. (c) Normalized light curves of the AIA 1600 Å and six EUV wave bands calculated in the FOV of the above images.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: (a) Normalized age distributions p(τ ∣ [Fe/H]) for single stars, binned in [Fe/H] and smoothed using Gaussian filtering. Each vertical slice is normalized by its peak value. The blue line marks the peak age in each bin. Colored points show planet-hosting stars, classified by guiding-center radius Rg: inner (Rg < 7.2 kpc), local (7.2 ≤ Rg​​ ≤ 9.2 kpc), and outer (Rg > 9.2 kpc). (b) Same as (a), but for [α/Fe] instead of [Fe/H].
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Comparison of [Fe/H] and [α/Fe] differences between stars hosting planets and nonhost stars with similar mass and age. (a) Scatterplot of differences in stellar age (ΔAge) versus stellar mass (ΔMass) between host stars and their nearest nonhost stars. (b) Distribution of host stars in the [Fe/H] versus [α/Fe] plane, colored by the difference in [Fe/H] between hosts and matched nonhosts.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Age precision and distribution of 18,990 sample stars. (a) Two-dimensional histogram of stellar age versus age uncertainty, with dashed lines indicating fractional age uncertainties of 10%, 20%, 30%, 40%, and 50%. The colorbar indicates the number of stars per bin in logarithmic scale. (b) Age histogram (gray bars) overlaid with a kernel density estimation (KDE)-smoothed curve (red). Vertical dashed lines and arrows highlight the detected peaks in the age distribution.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Kiel diagram of all LAMOST–Kepler–Gaia sample stars. Dwarfs, subgiants, and giants are shown in blue, orange, and red, respectively, based on classification with the evolstate algorithm. The black open circles indicate the location of our final sample of 18,890 stars with well-constrained ages.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Host star metallicity [Fe/H] as a function of planet radius for different stellar age groups. Each dot represents an individual host star, color-coded by age: black for young stars (≤5 Gyr), blue for intermediate-age stars (5–10 Gyr), and red for old stars (>10 Gyr). A small horizontal jitter (≤0.1) is added to the planet radius to reduce point overlap. The background boxplots show the distribution of [Fe/H] in each planet radius category across all ages. Segmented linear regression fits are overplotted for small planets (≤4 R⊕, green) and large planets (>4 R⊕, dark red), with shaded areas representing 1σ uncertainties of the fit. Pearson correlation coefficients (r) and p-values are indicated in red text. Sample sizes per bin are labeled above the boxplots, and planet radius classifications are noted along the bottom.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Cumulative distribution functions (CDFs) of elemental abundances for stars with and without planets, separated by stellar age and [Fe/H] bins. Only elements exhibiting statistically significant differences (p < 0.05) in a given bin are shown. Planet-hosting stars are indicated in red, and single stars in blue. Each subplot corresponds to one age bin (rows) and one significant element (columns), with [Fe/H] bin, sample sizes, and KS p-value labeled above each curve. In addition, the mean difference in [α/Fe] between host and nonhost stars (〈Δ[α/Fe]〉 = 〈[α/Fe]host〉 − 〈[α/Fe]non−host〉) and the KS p-value for [α/Fe] are annotated in each subplot.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Elemental differences between planet-hosting and single stars across stellar age and [Fe/H] bins. Each point represents the p-value from a two-sample Kolmogorov–Smirnov (KS) test comparing the abundance distributions of stars with and without planets. Points with p < 0.05 indicate statistically significant differences.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Comparison of ages for the 2866 stars in the cross-matched sample between our dataset and the subgiant sample from M. Xiang & H.-W. Rix (2022). The black line indicates the 1:1 relation. The mean age offset is −12.9%, with a scatter of 10.8%.
Paper: Insights into Planet Formation from the Ages, Masses, and Elemental Abundances of Host Stars
Authors: Xunzhou Chen, Tiancheng Sun, Lifei Ye
Figure caption: Same as Figure 7, but for host star [α/Fe].
Paper: A Multiwavelength View of ρ Oph. I. Resolving the X-Ray Source between A and B
Authors: Sean J. Gunderson, Jackson Codd, Walter W. Golay, David P. Huenemoerder, John M. Cannon, J. Alex Fluegel, Philip E. Griffin, Nathalie C. Haurberg, Richard Ignace, Alexandrea Moreno, Pragati Pradhan, Alexis Riggs, James Wetzel, Claude R. Canizares
Figure caption: Top panel: XMM MOS1 event file from Obs ID 0760900101 showing the reference stars used for correcting the aspect solutions in the X-ray observations. Bottom panels: images from Chandra ACIS-S, RLMT, XMM MOS1 (in order of observation date), and VLA. Images are centered to the same WCS coordinate with north up and east to the left but have different scales. ρ Oph A’s and B’s positions are marked with 2” radius regions in each image, B being northwest of A. For Chandra and RLMT, the optical positions are used. For XMM, the presented regions are corrected source positions. Regions in the VLA use the uniform beam shape (shown as the solid ellipse) and have corrected source positions. See Table 3 for corrective values.
Paper: A Multiwavelength View of ρ Oph. I. Resolving the X-Ray Source between A and B
Authors: Sean J. Gunderson, Jackson Codd, Walter W. Golay, David P. Huenemoerder, John M. Cannon, J. Alex Fluegel, Philip E. Griffin, Nathalie C. Haurberg, Richard Ignace, Alexandrea Moreno, Pragati Pradhan, Alexis Riggs, James Wetzel, Claude R. Canizares
Figure caption: Top: concatenated Chandra light curve in observation order with 2 ks time bins. Bottom left: NuSTAR FPMA (black) and XMM PN (magenta; Obs Id 0870920101) light curves with 1 ks bins. Bottom right: NuSTAR FPMA (black) and XMM PN (red; Obs Id 0720690101, blue; Obs Id 0760900101, and magenta; Obs Id 0870920101) light curves with 1 ks bins phased to the beginning of Obs Id 0720690101 assuming a 1.205 day period.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Top left: the rest-frame UV-optical SEDs of non-LRD broad Hα emitters GLASS 160133 and GLASS 150029 based on the JWST/NIRCam wide-band photometry from the UNCOVER DR3 “SUPER” photometry catalog. Top right: same as the left panel, but for LRD broad Hα emitters MSAID2008, MSAID4286, and MSAID38108. The vertical axis is the observed AB magnitudes shifted by ﹩5\mathrm{log}({d}_{L}/10\,\,\rm{pc}\,)﹩ where dL is the luminosity distance, and the horizontal axis is λrest = λobs/(1 + zspec). The filled symbols denote the observed magnitudes, and open symbols denote the magnitudes after subtracting the Hβ, [O III], and Hα emission-line flux contribution (Table 3). Bottom panels: same as the top panels, but the absolute magnitudes are K corrected relative to a reference redshift of z = 5 (see text in Section 2.1).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩52 × 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩52 NIRCam color image stamps of the JWST broad Hα emitters studied in this work, created from the all-epoch coadd images (see Section 2.2). The color coding is based on the F115W (blue), F150W (green), and F200W (red) images in the left column, and F277W, F356W, and F444W images in the right column. The marked positions indicate the putative AGN locations (brightest spots in each of the objects).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: The NIRCam all-epoch mosaic images of the A2744 field created from the multiband multiepoch data used in this study (see Section 2.2 and Table 1). Dashed lines in each panel denote the image footprints of the corresponding band, color-coded by the observation dates. The positions of the JWST broad Hα emitters analyzed in this study are indicated by the + and × symbols (Y. Harikane et al. 2023’s non-LRD broad Hα emitters; and J. E. Greene et al. 2024’s LRD broad Hα emitters, respectively).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: NIRCam F115W − F200W versus F277W − F444W and F277W − F356W versus F277W − F444W color–color diagrams of LRD and non-LRD broad Hα emitters from Y. Harikane et al. (2023) and J. E. Greene et al. (2024). The photometry was taken from the CEERS and UNCOVER “SUPER” photometric catalogs (K. A. Suess et al. 2024; L. Wright et al. 2024). The broad Hα emitters analyzed in this study are indicated by the + and × symbols (Y. Harikane et al. 2023’s non-LRD broad Hα emitters; and J. E. Greene et al. 2024’s LRD broad Hα emitters, respectively). The solid green line and the red-dashed and dashed–dotted lines represent the photometric LRD selection criteria defined by J. E. Greene et al. (2024): the green line marks the v-shaped SED selection window, and the red-dashed line (F277W − F444W > 1) and dashed–dotted line (F277W − F356W > 0.7) indicate the selection criteria for the red AGN continua.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Panels (a)–(e): 2.2 Msec Chandra/ACIS 0.5–7 keV X-ray coadded count images centered on the JWST broad Hα emitters (15″ × 15″, 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩492 pixel−1). The color bar indicates the X-ray counts from 0 (white) to 5 (black) counts. The source extraction aperture (r = 1″) and background extraction annulus (rin = 3″ and rin = 6″) are shown as solid and dotted lines, respectively. Panel (f): the X-ray coadded count image over the entire A2744 field. The background level is significantly elevated by the emission of the intracluster medium for objects close to the cluster cores (especially around MSAID38108).
Paper: A Multiwavelength View of ρ Oph. I. Resolving the X-Ray Source between A and B
Authors: Sean J. Gunderson, Jackson Codd, Walter W. Golay, David P. Huenemoerder, John M. Cannon, J. Alex Fluegel, Philip E. Griffin, Nathalie C. Haurberg, Richard Ignace, Alexandrea Moreno, Pragati Pradhan, Alexis Riggs, James Wetzel, Claude R. Canizares
Figure caption: Top panel: total Chandra HEG+MEG spectrum (black) and RGS1+RGS2 (blue) with best-fitting two-temperature plasma model (red and green) during quiescence. Both spectra have been binned by a constant factor of 10. Middle panel: NuSTAR FPMA+FPMB (black) with best-fitting one-temperature plasma model (red), binned by a constant factor of 3. Bottom panel: XMM PN (magenta), MOS1+MOS2 (black), and RGS1+RGS2 (blue) with best-fitting two-temperature plasma model (red, cyan, and green, respectively). The PN and MOS spectra are binned by a constant of 3, while RGS is binned by 10.
Paper: A Multiwavelength View of ρ Oph. I. Resolving the X-Ray Source between A and B
Authors: Sean J. Gunderson, Jackson Codd, Walter W. Golay, David P. Huenemoerder, John M. Cannon, J. Alex Fluegel, Philip E. Griffin, Nathalie C. Haurberg, Richard Ignace, Alexandrea Moreno, Pragati Pradhan, Alexis Riggs, James Wetzel, Claude R. Canizares
Figure caption: Zeroth-order Chandra ACIS-S spectrum of ρ Oph A (black) with best-fitting power-law DEM model (red). The spectrum of the background region is shown in gray.
Paper: A Multiwavelength View of ρ Oph. I. Resolving the X-Ray Source between A and B
Authors: Sean J. Gunderson, Jackson Codd, Walter W. Golay, David P. Huenemoerder, John M. Cannon, J. Alex Fluegel, Philip E. Griffin, Nathalie C. Haurberg, Richard Ignace, Alexandrea Moreno, Pragati Pradhan, Alexis Riggs, James Wetzel, Claude R. Canizares
Figure caption: The 90% line width contours of ρ Oph (solid) compared to the known unresolved line widths of HR 1099 (dashed).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Schematic pictures of possible scenarios for the nonvariable rest-frame optical continuum and broad Hα emission line in the JWST broad Hα emitters. The insets within the figure show an outline of the optical continuum + broad Hα spectral components (color-coded). Scenarios (a), (b), and (c) require an AGN, while scenario (d) is a non-AGN model (Section 4.3). We require the JWST broad Hα emitters to be X-ray faint (Section 4.1). (a): the continuum and broad Hα line are (moderately reddened) direct AGN emissions, but unlike typical AGNs, they do not exhibit flux variability for some reason. Compton-thick materials (e.g., BLR gas clouds) hide the X-ray corona, but do not obscure the accretion disk continuum. (b): the AGN disk continuum is dust obscured, but the AGN BLR emission is unobscured due to some specific geometry of the dusty materials, and the observed continuum is host stellar light dominated. Compton-thick materials (e.g., BLR gas and dusty clouds) hide the X-ray corona. (c): the observed spectrum is dominated by the scattered AGN disk continuum and scattered BLR Hα emission line, and the direct AGN emission is obscured. The scattered emission can be moderately reddened due to dust extinction inside the scattering regions. Compton-thick materials with a high covering factor hide the X-ray corona from both the observer and the scattering regions. This model requires an intrinsically superluminous AGN embedded inside the dusty materials (as indicated by dashed lines in the inset). (d): the continuum is the stellar light, and the broad Hα emission line is from either ultrafast and dense/low-metallicity stellar outflows or inelastic Raman scattering of stellar UV continua by neutral hydrogen atoms. This model is intrinsically X-ray faint unless there are ultraluminous stellar X-ray sources.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: The asymptotic variability amplitude ﹩{\rm{SF}\,}_{\infty }=\sqrt{2}{\sigma }_{\,\rm{d}}﹩ as a function of MBH. The gray dots denote the SDSS Stripe82 five-band data (u, g, r, i, and z band) of SDSS quasars (C. L. MacLeod et al. 2010), and blue points denote the ZTF g-band data of low-z dwarf AGNs (C. J. Burke et al. 2023). The downward arrows indicate the conservative upper limits on SF∞(4000Å) at the 90% confidence level obtained for GLASS 160133, GLASS 150029, MSAID2008, MSAID4286, and MSAID38108 (from left to right; see Section 3.2). The thick solid and thin dashed lines indicate C. J. Burke et al. (2023)’s empirical MBH-dependent model of SF∞, with Lbol/LEdd = 0.1 and varying host dilution covering factors f* = 0.2%–100%.