adsabs/AstroCLIMB huggingface dataset:
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The MFs of subfields. The upper panels are for CIC+MFs, and the lower panels are for DTFE MFs. From left to right, each panel shows cases of the halo number density of ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, ﹩1.6\times {10}^{-3}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, and ﹩1.6\times {10}^{-4}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, respectively. For each panel, we show 100 sets of MFs, which are randomly selected from the MFs of 512 subfields. Here, each V  i  has n b = 64 data points, and the unshielded regions indicate the density threshold ranges actually used in our calculations for Fisher forecasts (see Table 1).
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The mean RSD S/Ns. They are obtained by taking the average of ﹩\left|{\rm{\Delta }}{{\rm{V}}}_{i}\right|/{\sigma }_{i}﹩ (see Figure 13) in the density threshold range of [0.003, 1000], i.e., ﹩\overline{\left|{\rm{\Delta }}{V}_{i}\right|/{\sigma }_{i}}﹩. The results for the CIC+GS and DTFE MFs are marked with blue circles and red diamonds, respectively. As shown, the y-axis values of red diamonds are much higher than those of the blue circles, by around 2 orders of magnitude. This means that the discriminative power of DTFE MFs for RSD effects is much stronger than that of CIC+GS MFs.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The DTFE MFs of uniform-weighted halo fields in real space and redshift space. The corresponding halo number density for these fields is ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩. The solid and dashed lines represent the MFs in real and redshift space, respectively. As a reference, V 3 with linear Kaiser’s effect is also plotted (see the dotted line). As shown, the main RSD effect on MFs is the reduction in amplitudes of V 1, V 2, and V 3.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The same as Figure 11, but for the case of n b = 64.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The DTFE MFs of various weighted halo fields (see Figure 6) in real space. The corresponding halo number density for these fields is ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩. The yellow, blue, and red lines are for the uniform-weighted, mass-weighted, and optimally weighted halo fields, respectively.
Paper: Enhancing Morphological Measurements of the Cosmic Web with Delaunay Tessellation Field Estimation
Authors: Yu Liu, Yu Yu, Pengjie Zhang, Hao-Ran Yu
Figure caption: The correlation matrices for the DTFE MFs of uniform-weighted halo fields with different number densities. From left to right, each panel shows the case of the halo number density of ﹩1.6\times {10}^{-2}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, ﹩1.6\times {10}^{-3}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, and ﹩1.6\times {10}^{-4}{({h}^{-1}\,\mathrm{Mpc})}^{-3}﹩, respectively.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The normalization process using the continuum-fitting method. LAMOST-MRS spectra are drawn with the solid black lines; the left panels show the blue arm spectra, while the right panels display the red arm ones. The solid purple lines represent the pseudocontinuums, and the dashed purple lines indicate the upper and lower limits, which are used to exclude the emission and absorption lines. The identified cosmic rays are drawn with the orange lines. (a) The first fitting process, the initial continuum is fitted. (b) The second fitting process, the LAMOST-MRS spectrum is divided by the pseudocontinuum, and the green crosses denote the data points selected for local polynomial regression fitting. (c) The third fitting process, the pseudocontinuums are further refined. (d) The final normalized spectrum with the cosmic rays excluded.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distribution of uncertainties for the stellar parameters T eff, ﹩\mathrm{log}g﹩, and [Fe/H]. The S/Ns of spectral are drawn with different colors. The orange histogram represents the uncertainties of spectra with 10 < S/N < 30, purple for 30 < S/N < 50, green for 50 < S/N < 100, while blue for S/N > 100.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: Upper panels: the left panel is the H-R diagram of calibrated LAMA stellar parameters, middle panel is [Fe/H] vs. T eff, and the right panel is [Fe/H] vs. ﹩\mathrm{log}g﹩. Lower panels: the number of stars as functions of calibrated LAMA stellar parameter of T eff, ﹩\mathrm{log}g﹩, [Fe/H], and ﹩v\sin i﹩.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distribution of uncertainties for the stellar parameters of T eff, ﹩\mathrm{log}g﹩, and [Fe/H]. The number of visits are drawn with different colors.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distribution of resolution of the LAMOST-MRS blue and red arm spectra. The peak values of resolution for both the blue and red arm spectra are higher than 7500. Additionally, the scatter of resolution is larger for the blue arm spectra compared to the red spectra.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distribution of uncertainties for ﹩\mathrm{log}g﹩. It is obvious that the uncertainties of giants are larger than those of dwarfs.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The differences in parameters between GALAH and LAMA as a function of T eff. The cyan lines represent the average differences for each group of data. The red dashed lines indicate the fitted cubic polynomial curves.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The LAMOST-MRS resolutions of 4000 fibers of each night. The resolutions vary with dates and fibers.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The distribution of χ 2 for the blue and red arm spectra.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The number of stars vs. the number of visits.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: The g − i color vs. redshift for extragalactic NSS80 sources with reliable counterpart associations (also excluding those that are possibly associated with the primary NuSTAR science target), plotted in the different spectroscopic classifications: BL objects (blue circle), NL objects (green circle), unclassified sources (peach circle), galaxies (Gxy; peach “×”), AGN–galaxy pairs (peach star), dual AGN (purple star), and sources with uncertain counterpart identification (white filled circles with green and blue edges). The AGN–galaxy and dual AGN companions are plotted with white filled stars with peach and purple edges, respectively. BL and NL sources with L 10−40 keV ≥ 1044 erg s−1 are indicated with dark blue and green circles, while the light blue and green circles codify the lower-luminosity BLs and NLs with L 10−40 keV < 1044 erg s−1. SDSS-selected rQSOs (reddest 10% of the g − i distribution; K19) are superimposed on the distribution of the SDSS DR7 uniform sample (shaded gray circles). We use the rQSO track to identify 106 red NSS80 BL sources; of these, 67% (71/106) are at redshifts z ≤ 1. Using the same track, we identify a control sample comprising 145 BL AGN (52%, of which are at z ≤ 1). There is a bias against NLs at higher redshifts, given that all NLs (with constrained g and i magnitudes) are at z ≤ 1.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: WISE color–color diagram for the extragalactic NSS80 sources color coded by X-ray luminosity and spectroscopic classification following the color scheme in Figure 29: BL objects (blue circle), NL objects (green circle), and AGN–galaxy pairs (peach star). BL and NL sources with L 10−40 keV ≥ 1044 erg s−1 are indicated with dark blue and green circles, while the light blue and green circles codify the lower-luminosity BLs and NLs with L 10−40 keV < 1044 erg s−1. The Mateos et al. (2012) wedge, which identifies AGNs with red MIR power-law SEDs with a spectral index α ≤ −0.3, is indicated with a solid black line. We also compare with the AGN color cut of Stern et al. (2012, W1 − W2 > 0.8; black dotted line). In the top panel we show the WISE colors of the BL AGNs subdivided into low (light blue) and high (dark blue) L 10−40 keV. Our identified Nu-rQSOs (i.e., red BL AGNs) based on their g − i color are plotted with red stars; see Section 4.3 and Figure 29. The bottom panel shows the WISE colors for the  NuSTAR   NLs separated into L 10−40 keV < 1044 erg s−1 (light green) and L 10−40 keV ≥ 1044 erg s−1 (dark green). Two AGN–galaxy pairs are plotted with peach stars and two galaxies with white crosses.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: The bolometric luminosity–redshift plane for the (spectroscopically reliable) extragalactic NSS80 sources compared to SDSS optical quasars. The bolometric luminosity (L bol) for the NSS80 sources is inferred from the rest-frame 10–40 keV luminosity using a bolometric correction of BC = 25 (assuming that L 10−40 keV makes up ∼4% of L bol). Following the color scheme in Figure 29, the following subsamples are plotted: BL objects (blue circle), NL objects (green circle), unclassified sources (peach circle), galaxies (Gxy; peach “×”), AGN–galaxy pairs (peach star), dual AGN (purple star), and sources with uncertain counterpart identification (white filled circles with green and blue edges). The g − i-selected rQSOs (see Figure 29) are highlighted with red stars and the SDSS DR7 quasars are plotted using shaded gray circles. Compared to the optically selected SDSS quasars, the X-ray-selected  NuSTAR   serendipitous sources are typically ∼0.3 dex less luminous. The gray dotted line indicates the X-ray quasar threshold of L 10−40 keV = 1044 erg s−1. The median L bol for the extragalactic NSS80 sample is 7.19 × 1044 erg s−1 at the median redshift of the NLs (〈z NL〉 = 0.3), and 5.94 × 1045 erg s−1 at the BL median redshift (〈z BL〉 = 0.82), as indicated with green and blue dashed–dotted lines, respectively. Gray lines show kernel density estimation contours of the SDSS DR7 quasars at 68%, 95%, and 99.7%, for comparison with the distribution of NSS80 sources.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Composite spectra of the spectroscopically confirmed NSS80 BL (top panel; N stack = 274) and NL (middle panel; N stack = 166) samples. The BL sample is subdivided (bottom panel) into typical quasars (Nu-cQSO; solid blue line) and red quasars (Nu-rQSO; solid peach line). First, we compare to composite X-Shooter spectra of SDSS quasars, plotted with red and blue dotted lines (Fawcett et al. 2022). The signature AGN emission lines and galaxy absorption lines are plotted with gray dotted and dashed lines, respectively. We also compare to a composite of SDSS Type II AGNs from Yuan et al. (2016; purple dotted line). The spectra are shifted to rest-frame wavelengths and normalized at 4000 Å for illustrative purposes. The source threshold when (geometric mean) stacking the data is 15. Evidence for a larger host-galaxy contribution in the NuSTAR objects compared to SDSS are visible, while toward shorter wavelengths strong evidence for reddening in the NL objects, as well as some in the BL AGNs, can be seen.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Rest-frame 10−40 keV luminosity (L 10−40 keV) vs. redshift for the extragalactic NSS80 sources with reliable counterparts, separated into different spectroscopic classes: broad emission-line objects (BL; blue circle), narrow emission-line objects (NL; green circle), unclassified sources (peach circle), galaxies (Gxy; peach “×”), AGN–galaxy pairs (peach star), dual AGN (purple star), and sources with uncertain counterpart identification (white filled circles with green and blue edges). For comparison, the BASS DR2 (Koss et al. 2022) is plotted with gray crosses. The Swift-BAT 14−150 keV fluxes were used to calculate L 10−40 keV values assuming an effective photon index of Γeff = 2.0 for the K-correction factor. The gray dashed–dotted lines indicate an observed-frame X-ray flux range of 0.02–2 × 10−12 erg s−1 cm−2, i.e., spanning 2 orders of magnitude. The black dashed–dotted line highlights the evolution of the knee of the X-ray luminosity function (L *) with redshift (Aird et al. 2015).
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption:  NuSTAR   band ratio (BRNu) vs. redshift for the NSS80 sources, color coded by source classification: Galactic sources (z = 0; gray circle), broad emission-line objects (BL; blue circle), narrow emission-line objects (NL; green circle), unclassified sources (peach circle), galaxies (Gxy; peach “×”), AGN–galaxy pairs (peach star), dual AGNs (purple star), and highly obscured AGNs observed in NSS40 (red diamond; Lansbury et al. 2017a). Sources associated with the primary NuSTAR science target are excluded. BRNu values with upper or lower limits are faded using the respective classification colors. The dashed lines show tracks for a simple absorbed power-law model (assuming Γ = 1.8) and Galactic absorption of N H,Gal = 1020 cm−2 for a range of column densities along the line of sight to the nucleus. The distribution of constrained band ratios for the full NSS80 sample is shown on the right in faded gray, overlaid with the distribution of the BL (filled blue) and NL (open green) objects. The median constrained band ratio of the NSS80 sample is ∼0.8.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Composite spectra of the spectroscopically confirmed NL AGN (top), Nu-cQSO (middle), and Nu-rQSO (bottom) subdivided into low (light green, light blue, and peach, respectively) and high (dark green, dark blue, and red, respectively) luminosity bins. As in Figure 30, we compare to composite X-Shooter spectra of SDSS quasars, plotted with red and blue dotted lines (Fawcett et al. 2022), and composite spectra of SDSS Type-2 QSOs (Yuan et al. 2016), plotted with a purple dotted line. The signature AGN emission lines and galaxy absorption lines are plotted with gray dotted and dashed lines, respectively; see Figure 32 for zoom ins of the spectral lines. The spectra are shifted to rest-frame wavelengths and normalized at 4000 Å for illustrative purposes.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: The  NuSTAR   8−24 to 3−8 keV band ratio (BRNu) vs. full-band (3−24 keV) count rate for the NSS80 sources. Constrained BRNu values are shown in black, and those with upper or lower limits are shown in gray. The dotted horizontal lines indicate the equivalent X-ray spectral slope (Γeff) for a given band ratio. Highly obscured NSS40 serendipitous sources (Lansbury et al. 2017a), with BRNu values that correspond to Γeff < 0.7, are marked with red diamonds. The blue diamonds and the green circles show the median BRNu value per count rate bin of size 1 × 10−3 s−1 for the NSS40 and NSS80 sources, respectively.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Redshift distribution for the 433 spectroscopically identified extragalactic NSS80 sources with reliable counterpart identifications (light purple), excluding 19 sources with evidence for being associated with the NuSTAR targets for their respective observations. Left panel:  the distribution for the subset of NSS80 sources which are independently detected in the hard band (8−24 keV; dark purple). Right panel:  the redshift distribution separated by spectroscopic classification: BL objects are shown in blue, NL objects are shown in green, and “Other” (including four galaxies and two unclassified sources) are shown in peach. The vertical lines mark the median redshifts for the respective subsamples.
Paper: LAMA: LAMOST Medium-Resolution Spectral Analysis Pipeline
Authors: Chun-qian Li, Jian-rong Shi, Hong-liang Yan, Zhong-rui Bai, Jiang-tao Wang, Ming-yi Ding
Figure caption: The comparisons of stellar parameters between LAMA and APOGEE. Upper panels: the relations between LAMA stellar parameters and APOGEE results. Lower panels: The number stars as functions of the differences between the LAMA stellar parameters and those from APOGEE, and the Gaussian profiles are the fitting results. The values of mean μ and variance σ of Gaussian profiles are listed in the panels.