adsabs/AstroCLIMB huggingface dataset:
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 2003 (panel (a)) and 2004 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The averaged count distributions are normalized per 1° bin here for visualization purposes only, to show the PUI cutoff location with respect to each distribution function.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 2005 (panel (a)) and 2006 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The averaged count distributions are normalized per 1° bin here for visualization purposes only, to show the PUI cutoff location with respect to each distribution function.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 2007 (panel (a)) and 2008 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The averaged count distributions are normalized per 1° bin here for visualization purposes only, to show the PUI cutoff location with respect to each distribution function.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center years 2001 (panel (a)) and 2002 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the averaged combined counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center years 2003 (panel (a)) and 2004 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the averaged combined counts.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Time lag measurements for IC 4329A. The left panels show the photometric (top) and Hβ (bottom) light curves for each observing season. The photometric light curves are converted from magnitudes, normalized by their means, and rebinned using 1 day bins. The gray shaded bands represent reconstruction using MICA. In the panel showing the Hβ light curves, the black, blue, and green points represent the observed data from CAHA, LJ, and SAAO, respectively. The Hβ fluxes are in a unit of 10−13 erg s−1 cm−2. The right panels show autocorrelation functions (ACFs) of the photometric light curves (top) and interpolated cross-correlation functions (ICCFs) between the photometric and Hβ light curves (bottom). The blue histograms show the cross-correlation centroid distributions (CCCDs) from ICCF and yellow histograms show the posterior distribution of time lags from MICA. The gray shaded areas outline the region with the ICCF above 80% of the peak value, which is used for calculating the centroid time lag. In the 2020 season, the Hβ data point at JD 2459006 marked by an open circle is treated as an outlier (due to a telescope tracking issue) and is excluded in time lag analysis.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The mean and rms spectra over the whole monitoring period. For each object, the top and bottom panels show the mean and rms spectra, respectively. The red lines correspond to spectra after subtracting all other spectral components except for the Hβ and Hγ lines. The blue lines correspond to spectra without subtraction of the other spectral components. All spectra are in units of 10−14 erg s−1 cm−2 Å−1. Note that all spectra have been corrected for Galactic foreground and intrinsic extinction.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Examples of the spectral decomposition. For each object, the left panels show the spectral fitting with various components and the residuals. Gray shaded bands represent the fitting windows. The right panels show the extracted Hβ line and the spectral window adopted for calculating the integrated Hβ flux. The flux densities F  λ  are all in units of 10−14 erg s−1 cm−2 Å−1. Note that all spectra have been corrected for Galactic foreground and intrinsic extinction.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center year 2009 (panel (a)) and all combined years (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the averaged combined counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center years 2005 (panel (a)) and 2006 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the averaged combined counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center years 2007 (panel (a)) and 2008 (panel (b)). The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the averaged combined counts.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: Intercalibrated photometric light curves. The reference data set of intercalibration is by default adopted to be the ZTF g-band photometry for Mrk 335, Mrk 509, Mrk 1239, and PDS 456. For IC 4329A, there are no available ZTF data and the ASAS-SN g-band photometry is chosen as the reference data set. Gray shaded bands represent the spectral monitoring periods.
Paper: Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Yan-Rong Li, Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Hua-Rui Bai, Sen Yang, Pu Du, Feng-Na Fang, Yi-Xin Fu, Jun-Rong Liu, Yue-Chang Peng, Yu-Yang Songsheng, Yi-Lin Wang, Ming Xiao, Shuo Zhai, Hartmut Winkler, Jin-Ming Bai, Luis C. Ho, Romain G. Petrov, Jesús Aceituno, Jian-Min Wang
Figure caption: The light curves of the integrated Hβ fluxes over the whole monitoring period.
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: Upper left-hand panel: Background-subtracted, exposure-corrected surface brightness profiles of the jet in different energy bands. The error bars are at 1σ confidence level. For clarity, the profile in 0.5–6 keV is multiplied by a factor of 10. Upper right-hand panel: Hardness ratio profile defined as the ratio of the count in the soft energy band to the count in the hard energy band (Park et al. 2006). The larger the hardness ratio, the softer the emission. Errors are calculated using standard error propagation procedures. The red data point, calculated using a large region, represents the average value across the brighter part of the jet. The jet emission appears to be softer beyond 1.″2, but this could be due to soft emission from the galaxy or subject to systematic uncertainties. Bottom left-hand panel: Photon index vs. hardness ratio corresponding to the Chandra observation, assuming a power-law model absorbed by the Galactic column density. Bottom right-hand panel: Similar to the upper right-hand panel but the hardness ratio has been converted to photon index (thin black and red crosses) using the figure in the bottom left-hand panel. The low photon index at 0.″7 appears to be an outlier (see text). The photon indices determined using the spectral fitting method are also shown (thick gray and brown crosses).
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: X-ray spectra with different models as listed in Table 1. POWERLAW models were used on the left-hand panels while CUTOFFPL models were included on the corresponding right-hand panels. Upper left-hand panel: The absorbed POWERLAW model of the NuSTAR spectra (black and red), taken from within a 30″ circular region centered on the X-ray peak, was jointly fitted with the Swift spectrum (blue). This approach was used to constrain the overall hard X-ray emission originating from AGN activities (Core+Jet). The dotted lines represent the individual components (POWERLAW+APEC) as discussed in the text. Upper right-hand panel: Similar to the upper left-hand panel, but with the CUTOFFPL model replacing the POWERLAW model. Middle left-hand panel: Similar to the upper left-hand panel but including the Chandra jet spectrum (cyan) modeled with POWERLAW. The flux corrected jet models for the NuSTAR and Swift spectra are shown as dotted lines. The unresolved core is also modeled as a POWERLAW (dashed lines). Middle right-hand panel: Similar to the middle left-hand panel but with the CUTOFFPL model replacing the POWERLAW model for the unresolved core. Lower left-hand panel: Similar to the middle left-hand panel but including the Chandra core spectrum (magenta) modeled with POWERLAW. Middle right-hand panel: Similar to the lower left-hand panel but with the CUTOFFPL model replacing the POWERLAW model for the unresolved core.
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: Upper left-hand panel: 0.3–6 keV Chandra subpixel resolution image. The arc feature highlighted in the green region is an artifact of the Chandra PSF. The emission is elongated in the direction of the jet to the northeast. Upper right-hand panel: Deconvolved Chandra image in 0.3–6 keV. Lower panels: Deconvolved Chandra image in the wide band (0.5–6 keV; left-hand panel), soft band (0.5–1 keV; middle panel), and hard band (1–6 keV; right-hand panel). The regions shown on the left are used for the analysis of surface brightness and hardness ratio profiles. In all panels, the color bar units are counts per image pixel, and one image pixel size = 0.″0615. For each deconvolved image, the PSF artifact, located within the box region, has been excluded.
Paper: NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Ka-Wah Wong, Colin M. Steiner, Allison M. Blum, Dacheng Lin, Rodrigo Nemmen, Jimmy A. Irwin, Daniel R. Wik
Figure caption: Photon index fitted at various energy bins for different dataset. NuSTAR and Chandra data were fitted with absorbed POWERLAW model. For Swift data, since there is a clear soft excess, an absorbed APEC + POWERLAW model was used.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: (a) Distribution of distance from the filament spine (D fil) for all filament galaxies (black) with D fil ≤ 1 Mpc h −1, galaxies detected (blue), and undetected (red) in our UVIT FUV survey. (b) g − r vs. M  r  CMD for filament galaxies. The contour is composed of a sample of local galaxies observed in SDSS DR 16. (c) BPT diagram used to separate H II region galaxies from composite and Seyfert galaxies. The solid and dashed polynomials are described in Kewley et al. (2001) and Kauffmann et al. (2003a), respectively. Each gray dot represents a galaxy present in the Kauffmann et al. (2003b) spectroscopic catalog. (d) Gini coefficient vs. M20 coefficient for all filament galaxies. The markers have the same meaning as (a).
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: A limb apparent current sheet on 2001 September 21 (case 4; H. Q. Song et al. 2012). Panels (a1)–(a2): the SOHO/LASCO C2 images. The red dotted–dashed line in panel (a2) denotes a slit along the length direction of the current sheet, and the red solid lines represent the slits along the width direction. Panel (b1): the width (the blue histogram) and length (the red histogram) of the current sheet. The blue arrow denotes the thinning process of the current sheet. Panel (b2): the aspect ratio of the current sheet (see the black solid histogram). The solid histogram is fitted with a power-law function of the time-aspect ratio (see the black curve), and the temporal evolution of the aspect ratio of the current sheet follows a power law with exponent 2.35. Panel (c): a three-dimensional mesh surface displaying the normalized intensities within the green box in panel (a2).
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Redshift cone diagram showing the distribution of galaxies in the line-of-sight of UVIT observation. Each black dot in the figure represents a galaxy taken from SDSS DR 16. A blue rectangular box surrounds the filamentary structure observed in our UVIT survey. The inset plot displays the zoomed-in structure. The galaxy distribution in light-green color highlights one of the filaments (Filament ID 1029 in Tempel et al. 2014) studied in this work. The magenta and green lines enclose the UVIT FOVs observed in the present study. The red circle represents the boundary of the Bootes void, while the pair of blue lines encloses the FOV observed by us to examine the properties of void galaxies (Pandey et al. 2021).
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: Plasma and thermal distributions of the limb apparent current sheet in Figure 6. Panels (a)–(c): the EM (a), density (b), and temperature (c) maps. The white solid lines in panels (a)–(c) denote the normalized EM, density, and temperature variation curves along the current sheet, respectively. Panels (d)–(f): three-dimensional mesh surfaces displaying the EM, density, and temperature intensities of the maps in panels (a)–(c), respectively.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Left panel: comparison between SFRFUV and SFR144MHz for star-forming (circles) and AGN (crosses) filament galaxies. The color bar represents M ⋆. The dashed line indicates one-to-one correspondence between the quantities. Right panel: sSFR vs. M ⋆ for UVIT-detected (circles) and undetected (triangles) filament galaxies. The downward triangular markers indicate the upper limit of sSFRFUV. The AGN hosts are outlined with maroon crosses. The dashed line represents galaxies with SFR = 1 M ⊙ yr−1. The color bar represents the D fil for each galaxy. Background galaxies shown with gray markers are taken from Salim et al. (2016).
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: A moving blob within the limb apparent current sheet. Panels (a1)-(a3): the SDO/AIA EUV images in 131 Å wavelength. Panels (b1)–(d3): the EM ((b1)–(b3)), density ((c1)–(c3)), and temperature ((d1)–(d3)) maps. The white arrows denote the blob.
Paper: Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan
Figure caption: Sky map in a Cartesian grid defined by Tempel et al. (2014) showing the distribution of galaxies in our FOV. Our UVIT pointings are enclosed in rectangular boxes. The galaxies within 1 Mpc h −1 from the filament spine and the corresponding filament spine for each filament are shown with different symbols and colors. The detected galaxies in the FUV survey are outlined with blue crosses, whereas the red-colored crosses within FOVs represent filament galaxies that were FUV undetected. Gray markers show the background galaxies in the FOV from the SDSS survey.
Paper: Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Tao Ding, Jun Zhang
Figure caption: The evolution of the apparent current sheet in Figure 5. Panels (a1), (b1), and (c1) show the EM, density, and temperature maps of the current sheet, respectively, and panels (a2), (b2), and (c2) display the time–distance slits of the EM, density, and temperature maps along “S1” in panel (a1). The green rectangle in panel (a1) outlines the FOV in Figure 7.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: The first row presents the performance of the ANN considering the accuracy (left) and loss (right) evolutions during the training and validation phases. The second row presents the computed ROC curve (left) and confusion matrix (right) during the test phase.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: The angular separations of classified binaries presented as a function of the inverse of the system’s primary parallax. Both sets of misclassified (orange) and correctly classified (blue) binaries are overplotted by a Gaussian kernel density estimation. The binaries in the test set are denoted by the two contours, where the black and red contours correspond to the visual and true binary classes, respectively.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: Histogram of true and visual binaries in the sorted catalog as a function of their physical separation. The range of values falls between 0.70 < log(s au−1) < 5.31, obeying the initial condition of s < 206,265 au.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: Histogram of misclassified and correctly classified binaries from the test set as a function of their physical separation. The range of physical separations for misclassified binaries falls between 2.95 < log(s au−1) < 5.30, with values falling between 4.10 < log(s au−1) < 5.18 within ±3σ of the mean.
Paper: Astrometric Binary Classification via Artificial Neural Networks
Authors: Joe Smith
Figure caption: Physical separations plotted against their corresponding angular separations. Overplotted for true (blue) and visual (orange) binaries are 2D density histograms.