adsabs/AstroCLIMB huggingface dataset:
Paper: WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies
Authors: N. Deg, K. Spekkens, N. Arora, R. Dudley, H. White, A. Helias, J. English, T. O'Beirne, V. Kilborn, G. Ferrand, M. L. A. Richardson, B. Catinella, L. Cortese, H. Dénes, A. Elagali, B.-Q. For, K. Lee-Waddell, J. Rhee, L. Shao, A. X. Shen, L. Staveley-Smith, T. Westmeier, O. I. Wong
Figure caption: The successes and failures of 3DBAROLO FAT and WKAPP for a sample of 100 idealized VD galaxies generated by MCGSUITE. Panels and symbols are the same as those in Figure 3.
Paper: First X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 17+2
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Alexandra J. Tetarenko, Pau Bosch-Cabot, Herman L. Marshall
Figure caption: Left panel: contour plots of the polarization degree and angle, determined with the PCUBE algorithm, at the 68%, 95% and 99% confidence levels, in the 2–8 energy band. Right panel: contour plots of the polarization degree and angle, determined with the PCUBE algorithm, at the 68%, 95% and 99% confidence levels, in the 2–4 keV (blue), 4–8 keV (red), 4–6 keV (black), and 6–8 keV (orange) energy bands. The contour plots show no strong variation of the source PA/PD with energy, considering the uncertainties.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: A map of PPOs in W51-E. In the central panel, subfields containing PPOs are labeled. Cutout images of each labeled grid are displayed in the side panels. The positions of the PPOs are annotated by a arrow with their ID and color representing their classification (cyan: dust dominated, orange: dust + free–free, green: free–free contaminated, magenta: only found at 1.3 mm, and yellow: only found at 3 mm). The cyan crosses mark PPOs included in the W51-IRS2 catalog. The background image is a 3 mm long-baseline continuum image. The color scaling in each inset is individually adjusted for better visual clarity.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Snapshots of PPOs identified in the W51-E 1.3 mm and 3 mm continuum images. The color scale is normalized to the flux of the central object for clear visualization. The size of the image beam is represented as a filled ellipse at the left lower corner.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: The completeness test result. We define the completeness limit mass as the mass reaching the completeness level = 0.9. Each point is generated by testing if the synthetic sources are detected by dendrogram or not. The interpolation between points is done with PCHIP interpolator.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 25 continued.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Same as Figure 23 but for W51-IRS2. The cyan crosses mark the PPOs in the W51-E catalog.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 28 continued. The images of undetected sources in the dendrogram are surrounded by cyan squares.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 23 continued.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 28 continued.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 37 continued. The sources #4–#10 are outside of the field of view of the 1.3 mm continuum image.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Snapshots of ambiguous sources that were not selected in the final catalog of PPOs in W51-E. The cyan square indicates the absence of the sources in the ambiguous object catalog.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Snapshots of PPOs identified in W51-IRS2 1.3 mm and 3 mm continuum images. Sources #32–39 do not have a counterpart in the 1.3 mm field of view.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Snapshots of low-S/N sources in W51-E. Sources #2–#7 are outside of the field of view of the 1.3 mm continuum image.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Snapshots of ambiguous sources in W51-IRS2. The sources #27–#32 are outside of the field of view of the 1.3 mm continuum image.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 28 continued. For #107–117, the sky position of the 1.3 mm counterpart is out of the field of view.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 32 Continued. For #42–92, the sky position of the 1.3 mm counterpart is out of the field of view.
Paper: ALMA-IMF. XX. Core Fragmentation in the W51 High-mass Star-forming Region
Authors: T. Yoo, A. Ginsburg, J. Braine, N. Budaiev, F. Louvet, F. Motte, A. M. Stutz, B. Thomasson, M. Armante, M. Bonfand, S. Bontemps, L. Bronfman, G. Busquet, T. Csengeri, N. Cunningham, J. Di Francesco, D. J. Díaz-González, M. Fernández-Lopez, R. Galván-Madrid, C. Goddi, A. Gusdorf, N. Kessler, A. Koley, H.-L Liu, T. Nony, F. Olguin, P. Sanhueza, M. Valeille-Manet, L. A. Zapata, Q. Zhang
Figure caption: Figure 34 continued. The sources #43 and #44 are outside of the field of view of the 1.3 mm continuum image.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Left: N/O vs. He/H (left) and O/H (right) of PN G048.5+04.2 (green dot) and PN G068.7+14.8 (blue dot), along with values of the Sun (red ⊙; M. Asplund et al. 2009) and the Orion Nebula (black asterisk; C. Esteban et al. 2004). The symbols and color coding are the same as in Figure 10. Right: same as the left but for Ne/H vs. O/H. In the top panels, AGB model predictions from A. I. Karakas (2010; Z = 0.004), C. K. Fishlock et al. (2014; Z = 0.001), and A. I. Karakas & M. Lugaro (2016; Z = 0.007, 0.014 and 0.03) for surface abundances at different metallicities are overplotted for the purpose of comparison. In the bottom panels, AGB model predictions from P. Ventura et al. (2013; Z = 0.001) and P. Ventura et al. (2014; Z = 0.004) are overplotted. Different symbols represent different metallicities; symbols of the same metallicity are linked by dotted lines to aid visualization. The initial mass (in units of M⊙) of the progenitor star is labeled for each model. The vertical scales of the top and bottom panels are different to accommodate the AGB model grids.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Central-star positions of the two PNe in the H-R diagram. Overplotted in the diagram are the model tracks of the H-burning post-AGB sequences calculated by M. M. Miller Bertolami (2016; at Z = 0.02). Different line types represent different different initial and final masses. Red curves are the isochrones for the evolutionary ages (τ = 0, 5000, 10,000, 15,000, and 20,000 yr) since the beginning point of the post-AGB defined at ﹩\mathrm{log}{T}_{{\rm{eff}}}﹩ = 3.85.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: N/O vs. O/H (left) and He/H (right), both displayed in logarithmic scale. PN G048.5+04.2 (large green dot) and PN G068.7+14.8 (large blue dot) are compared with the samples from the literature as represented by different symbols (see the legend). Solar abundances are adopted from M. Asplund et al. (2009). Typical error bars of the literature samples are indicated in the bottom-left corner.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Observed intensities (normalized to I(Hβ) = 100) of high-order Paschen lines Pn (n ≥ 10) of H I, as measured from the GTC spectrum of PN G048.5+04.2 (top) and PN G068.7+14.8 (bottom), as a function of principal quantum number n. The various curves show the predicted Paschen decrements for electron densities from 102 to 106 cm−3, calculated at PJ temperatures of 9660 K (for PN G048.5+04.2, top) and 9390 K (for PN G068.7+14.8, bottom). The measurement uncertainties of the Paschen lines in PN G048.5+04.2 are relatively larger. Measurement of the P10 line in PN G068.7+14.8 is underestimated, probably due to oversubtraction of the nebular continuum. The intensities of P16 and P18 might be overestimated due to unknown blending.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: GTC/OSIRIS spectrum of PN G068.7+14.8; probable emission features from its W-R-type central star are labeled in red.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: GTC/OSIRIS R1000R spectrum of PN G048.5+04.2 (top) and PN G068.7+14.8 (bottom) in the wavelength region of 7800–9000 Å, showing the Paschen discontinuity at ∼8204 Å and the high-order Paschen decrements. The dashed curves overplotted are empirical fits to the continuum on both sides of the PJ; note that for PN G048.5+04.2, the continuum redward of the PJ of is obviously elevated due to contamination from a field star (as shown in Figure 1, top). Both spectra have been corrected for extinction and radial velocities, as determined through measurements of H I Balmer and Paschen lines.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Galactic radial oxygen gradients of the PNe (black symbols, samples adopted from B. Bucciarelli & L. Stanghellini 2023) with young progenitors (YPPNe, top panel) and old progenitors (OPPNe, bottom panel) as defined according to L. Stanghellini & M. Haywood (2018). PN G048.5+04.2 (green dot) and PN G068.7+14.8 (blue dot) are overplotted, with a 0.1 dex error bar in the oxygen abundance set for both; their RG values are adopted from B. Bucciarelli & L. Stanghellini (2023). In each panel, the red dashed line is a linear fit to the PN sample of B. Bucciarelli & L. Stanghellini (2023).
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Ne/H vs. O/H (top left), S/H vs. O/H (top right), Cl/H vs. O/H (bottom left), and Ar/H vs. O/H (bottom right), all displayed in logarithmic scale. Symbols are the same as in Figure 10. The typical error bars of the literature samples are indicated in the top-left corner.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Comparison of the observed and the model-predicted line ratios of PN G048.5+04.2 (top) and PN G068.7+14.8 (bottom) as listed in Table 12; [S II] λ6720 is a combination of the λλ6716, 6731 doublet . Differences are all <2.5%.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: Histogram of the offsets of the X-ray sources from the optical center of their host galaxies. We compare our distribution of 27 AGNs in gray to the expected values from J. M. Bellovary et al. (2019) in blue and the X-ray-selected AGN sample from A. Sacchi et al. (2024) in green. We find a larger number of sources with offsets between 1 and 2 kpc than expected, although we note that this histogram does not include the positional uncertainties of the X-ray source positions.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: DECaLS grz images of the eight galaxies in our sample with X-ray emission consistent with XRBs. Magenta crosses and circles show the positions and positional uncertainties of the X-ray sources from eRASS1. Green circles indicate the locations of the SDSS spectral fibers (with 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 radii) for the galaxies with SDSS spectra.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: Location of the 22 galaxies in our AGN sample with SDSS spectra on the BPT diagram. Only one galaxy (ID 1) is found outside the H II region of the diagram. The dividing lines in the diagram come from the classification scheme outlined in L. J. Kewley et al. (2006).
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: BH mass vs. X-ray luminosity of the 27 galaxies in our AGN sample. Lines of constant Eddington ratio are shown with light red lines. Two galaxies (IDs 7 and 18) have Eddington ratios above λedd = 1.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: WISE colors of the galaxies in our final AGN sample with reliable WISE detections. The D. Stern et al. (2012) cutoff is shown in blue, and the T. H. Jarrett et al. (2011) selection box is shown in red. We find that two of the galaxies (IDs 6 and 7) have colors consistent with mid-IR AGNs.
Paper: A New Sample of Dwarf Galaxies with X-Ray-selected Active Galactic Nucleus Candidates from the eROSITA All-Sky Survey
Authors: John-Michael Eberhard, Amy E. Reines
Figure caption: Histogram of the normalized offsets of the X-ray sources from the optical center of their host galaxies. We compare our AGN sample to the X-ray-selected AGN samples from K. L. Birchall et al. (2020) and A. Sacchi et al. (2024).
Paper: Luminosity Distance Dispersion in Swiss-cheese Cosmology as a Function of the Hole Size Distribution
Authors: T. Cheunchitra, A. Melatos, R. L. Webster
Figure caption: Luminosity distance dispersion as a function of Swiss-cheese hole size distribution. Each panel displays the standard deviation ﹩{\sigma }_{{D}_{{\rm{L}}}}﹩ as a function of the lower cutoff ﹩{R}_{{\rm{\min }}}﹩ (logarithmic vertical axis; ﹩{R}_{{\rm{\min }}}﹩ in units of Mpc) and exponent γ (horizontal axis; dimensionless) of the power-law hole size distribution for one redshift in the range 0.5 ≤ ztarget ≤ 2.1 per panel. In each panel, a pixel corresponds to a Swiss-cheese universe with standard parameters (see Table 1), ﹩{R}_{{\rm{\max }}}=70\,{\rm{Mpc}}﹩, ﹩{R}_{{\rm{\min }}}﹩ in the range ﹩-1\,\leqslant \,{\mathrm{log}}_{10}({R}_{{\rm{\min }}}/1\,{\rm{Mpc}})\,\leqslant \,1﹩, and γ in the range 1.1 ≤ γ ≤ 3.1. The color of each pixel displays ﹩{\sigma }_{{D}_{{\rm{L}}}}﹩ in units of Mpc in logarithmic scale (see color bar at right). For each universe, ﹩{\sigma }_{{D}_{{\rm{L}}}}﹩ is calculated using the method detailed in Section 4 from a sample of 50 (z, DL) pairs generated independently using the recipe in Section 4. For all Swiss-cheese universes, we have ﹩{R}_{{\rm{\max }}}=70\,{\rm{Mpc}}﹩, and all other parameters are listed in Table 1.
Paper: Luminosity Distance Dispersion in Swiss-cheese Cosmology as a Function of the Hole Size Distribution
Authors: T. Cheunchitra, A. Melatos, R. L. Webster
Figure caption: An illustrative example of the DL dispersion near ztarget = 2.1. Top panel: sample of 50 (DL, z) pairs in the range 2.05 < z < 2.20 in a Swiss-cheese universe with standard parameters (see Table 1), γ = 1.1, ﹩{R}_{{\rm{\min }}}=10﹩ Mpc, and ﹩{R}_{{\rm{\max }}}=70﹩ Mpc (black points). The color gradient displays the kernel density estimate of the normalized PDF p(DL, z) (see color bar at right). Although hard to discern by eye, the color gradient is roughly an ellipse, not a line. The gray dashed line marks z = ztarget. Bottom panel: slice of the PDF p(DL, ztarget) calculated by evaluating the kernel density estimate for z = ztarget. Note that p(DL, z) is normalized on the DL–z plane, but p(DL, ztarget) is an unnormalized slice of p(DL, z).