adsabs/AstroCLIMB huggingface dataset:
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Spectral distribution plot of the best-fit leptonic (blue) and hadronic (red) scenarios that have been fitted using the TeV γ-ray flux points speculated to have the same original source (H.E.S.S. Collaboration et al. 2018; Cao et al. 2021; Amenomori et al. 2022). The error bands indicate statistical errors.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Best-fit spectrum of HAWC J1844−034.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Collection of spectra for γ-ray sources within the vicinity of HAWC J1844−034. The results have been collected from Fermi-LAT (Abdollahi et al. 2020), H.E.S.S. (H.E.S.S. Collaboration et al. 2018), Tibet AS-Gamma (Amenomori et al. 2022), LHAASO (Cao et al. 2021), and HAWC.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: One-dimensional significance distribution histogram collected per pixel of Figure 2(b). The expected background-only distribution is described by the red Gaussian curve. The green line is the best-fit Gaussian curve of the data present in the range between −2 and 2.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Radial profile from the best-fit location of HAWC J1844−034 in the center. The dotted lines are the radial distances of the best-fit positions of the sources from the center of HAWC J1844−034.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: (a) Significance map of the best-fit model described in Table 1. (b) Residual map produced by subtracting the best-fit model.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: Component populations of proposed 25–35 Myr structures, which are extended along an axis perpendicular to known spiral structure. We display these structures in XY and XZ galactic coordinates, showing their spatial coherence, as well as l–v  T,l  space, in which continuous sinusoidal arcs typically indicate common velocities that are modulated by projection effects in l. Shades of orange are associated with Cep-Her, while shades of purple and blue are associated with Carina-Musca. We also include the near edge of the Vela complex in black, which has a similar age and location to Carina-Musca. Both proposed structures follow consistent arcs in both XY and XZ coordinates, with Cep-Her’s proposed structure being inclined to the galactic plane, while Carina-Musca’s structure is relatively flat. Cep-Her and its companions show a tight velocity trend in l, consistent with projections of a single common velocity. Carina-Musca has multiple components in l–v  T,l  space, indicating that it is less dynamically coherent, but it still shows a few continuous arcs, with the largest consisting of Carina-Musca, SCYA-111, P51, Theia 246, and part of Vela, which is similar to Cep-Her in its spatial extent. We show the projected median 3D velocity vectors of the δ Lyrae cluster in Cep-Her and Carina-Musca as red and blue curves, respectively, demonstrating relatively consistent velocities of these groups. These structures are prime targets for RV follow-up, which would enable the reconstruction of patterns in their formation sites via trace-back.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: The distribution of ages for stellar populations, presented in the XY plane, and limited to the inner 500 pc where patterns are visible for stars near 30 Myr. Annotations show the locations of the Radcliffe Wave, the Split, and our proposed older structures. The age distribution can also be interacted with in the online-only version of Figure 8, which allows the isolation of structures around 30 Myr, or the young structures (age < 20 Myr), which are plotted alongside the outlines of the Radcliffe Wave and the Split.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: The curve for the field population corrective factor, which is the inverse of the fraction of total field stars identified as old using P Age<50 Myr < 0.001 (see Figure 4). The increase in distance reflects the less reliable youth assessment of stars that are higher on the main sequence.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: Left: contours and false color map of the 6000 component. The dashed white lines delineate the stripe within which the data of the P–V plot (in the right panel) are taken. The yellow cross marks the sky position of x = 0 in the P–V plot, whose coordinates are 22h36m00.ˢ8 +33d57m47s. The width of the stripe is 5′ and the position angle is P.A. = 99°. Right: P–V plot. The contours start from 1 mJy beam−1 (beamwidth = 2.′9) with an increment of a factor of 2.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: (Top) FAST H I channel maps (contours) overplotted on a CFHT r-band image (Duc et al. 2018). The channel maps cover the velocity range of 5480–7040 km s−1 with a channel width of 20 km s−1. The contour levels are [3, 6, 12, 24, 48, 96...] × 4.2 × 1016 cm−2. The blue boundaries delineate the FAST coverage. The small red circle at lower left corner of the first map in the last row shows the angular resolution of the H I channel maps (FWHM = 4′). (Middle) and (bottom) Contours of the H I channel maps overplotted on the r-band image.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: Top panel: continuum-subtracted spectrum of the optical counterpart of Anon 9 between 6500 and 6950 Å observed wavelength. The red lines indicate the [N II], Hα, and [S II] positions at a redshift of 0.0195. Middle panel: 2D spectrum of Anon 9 with the wavelength range the same as the lower panel. Lower panel: 1D original spectrum. The dash lines show the positions of Hα and [S II] at z = 0.0195. The gray regions are contaminated by sky lines.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: Optical spectra. The gray regions are contaminated by sky lines.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: Clusters identified by HDBSCAN, shown in XY Galactic Cartesian coordinates and l/b Galactic sky coordinates marked by their vetting status. We introduce small differences in hue to distinguish overlapping groups, but we broadly use orange-ish shades marked by upward-facing arrows to represent real groups, while blueish shades marked by downward-facing arrows represent false groups. Real but older groups are shown as black circles. The extensive rays of false groups toward the right side of the XY plot are mainly produced by reddening anomalies in the foregrounds in Serpens, Aquila, and the Pipe Nebula.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: Figure showing the regions of the H-R diagram that we identified as reliably old (P Age<50 Myr < 0.001) or young (P Age<50 Myr > 0.2), using Sco-Cen as an example. Young stars are identified on the pre-main sequence and the tip of the OB sequence, and old stars are confidently identified on the lower-main sequence, giant branch, and white dwarf cooling sequence. The faintness of most stars in those reliably young or old sets makes the fraction of the respective populations that they represent a strong function of distance once faint stars begin to become invisible to Gaia.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: A Hertzsprung–Russell diagram demonstrating our sample model using the new DR3 photometric system. This example uses a distance of 500 pc for merging binaries, although we also generate 938 other models for comparison with stars at different distances. Like in SPYGLASS-I, there are some streak-like density anomalies on the giant branch and far upper main sequence. These are caused by the speed of stellar evolution in these regions; however, youth is typically not contentious there, so sampling density issues are unlikely to be important.
Paper: SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Authors: Ronan Kerr, Adam L. Kraus, Aaron C. Rizzuto
Figure caption: The transverse velocity distribution for SCYA-6 (Circinus), which has high enough local reddening that a large sample of nonmember field stars is included in the founding population that follows a much broader velocity distribution compared to the group itself. Circinus is the only severe example of this; however, it demonstrates that in the most distant and most heavily reddened groups, harsher P mem restrictions that exclude some founding members may be desirable for future analysis. This velocity distribution can also be viewed in the online-only version of Figure 10.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: Contour maps of the integrated flux of the five kinematical components (see Figure 2) overplotted on an r-band image. The red contour levels are [4, 8, 16, 32, 64, ...] × σ, where ﹩\sigma =\sqrt{{\rm{\Delta }}v/20\,\mathrm{km}\,{{\rm{s}}}^{-1}}\times 4.2\times {10}^{16}\,{\mathrm{cm}}^{-2}﹩, and the velocity range of each component is provided in the corresponding panel. Marked on the maps are also the neighboring galaxies detected by the FAST observations (see Section 4). The red circle at the bottom-left corner of panel (a) shows the angular resolution of the contour maps (FWHM = 4.′0). The green contours in panels (a), (b), and (d) represent the VLA moment-0 maps in velocity ranges of 5597–5789 km s−1, 5959–6068 km s−1, and 6475–6755 km s−1, respectively. The contours levels are 5.8, 12, 18, 23, 29, 44, 58, and 73 × 1019 cm−1 for a synthesized beam of 19.″4 × 18.″6.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: Contour map (in blue contours) of the integrated H I emission between 5600–7000 km s−1 overplotted on an r-band image. The contour levels are [4, 8, 16, 32, 64, ...] × 3.5 × 1017 cm−2. The green boundary delineates the coverage of the FAST observations. The central red circle (﹩D=12^{\prime} ﹩) shows the aperture with which the total H I spectrum presented in Figure 2 is extracted. The orange line delineates the diffuse H I feature whose systemic velocity is written in brown labels (Xu et al. 2022). Provided in the figure is also information for the member galaxies and the main tidal features in SQ (in red labels), for neighboring galaxies detected by FAST (in blue labels) whose positions are marked by blue circles, and for the neighboring galaxy KAZ 295 (in blue labels). For each source, the name, Hubble type (when available), and velocity in km s−1 are listed.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: H I spectra of SQ obtained by FAST (red), Arecibo (green; Peterson & Shostak 1980), and GBT (blue; Borthakur et al. 2015). The red vertical dashed lines mark the boundaries of the five kinematical components. We have smoothed the Arecibo and GBT spectra to a resolution of 20 km s−1 for comparison, from their original resolutions of 8.8 km s−1 and 10 km s−1, respectively.
Paper: Deep H I Mapping of Stephan’s Quintet and Its Neighborhood
Authors: Cheng Cheng, Cong Kevin Xu, P. N. Appleton, P.-A. Duc, N.-Y. Tang, Y.-S. Dai, J.-S. Huang, U. Lisenfeld, F. Renaud, Chuan He, Hai-Cheng Feng
Figure caption: H I spectra of four neighboring galaxies. The dash gray lines show the position of zero flux. H I spectra of NGC 7320a and Anon 7 are presented in Xu et al. (2022).
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) Bolometric luminosities vs. L 3.4 values. The bolometric luminosities are adopted from Krawczyk et al. (2013). The blue-dotted line represents the relation when α and β in Equation (4) are set as free parameters, and the red-dashed line denotes the relation when the slope term β is fixed to 1. Gray dashed–dotted and dashed–dot–dotted lines denote the best-fit correlations derived with the AGN templates of Richards et al. (2006) and Assef et al. (2010), respectively, where α and β are treated as free parameters. (b) Bolometric luminosities vs. L5100 values. The meanings of the red-dashed and blue-dotted lines are identical to those in the left panel. The gray dashed–dotted line shows the relation of L5100–L bol by adopting the correction factor of 9.26 (Shen et al. 2011), which is measured based on the AGN template of Richards et al. (2006). The discrepancy between the red-dashed and blue-dotted lines is due to Richards et al. (2006) using a different wavelength range (100 μm–10 keV) to measure the bolometric luminosity from that used (1 μm–10 keV) by Krawczyk et al. (2013).
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) BH masses measured from L5100 and FWHMHβ  vs. M BH values from L 3.4 and FWHMHβ . The L MIR-based M BH estimator is derived by replacing the L5100 of the M BH estimator of Vestergaard & Peterson (2006) with the L 3.4. For replacing the L5100 of the M BH estimator, we use the linear relation of L5100–L MIR presented as the parameter set A in Table 1. The red-dashed line represents the case where the BH masses are identical. (b) Comparison of M BH values derived from the optical properties and the L 3.4-based BH masses. The L 3.4-based BH masses are measured as the left panel, but the parameter set C in Table 1 is used for the L5100–L MIR relation. The meaning of the red-dashed line is identical to that in the left panel.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) Comparison of L bol derived from the L 4.6 vs. L bol measured based on the L5100. The gray histogram represents the distribution of ΔL bol/L bol, which is (L bol,MIR − L bol,opt)/L bol,opt, and its distribution is clearly skewed toward higher values. (b) Comparison of M BH measured from the L 4.6 and the L5100. The gray histogram shows the distribution of ΔM BH/M BH, which is (M BH,MIR−M BH,opt)/M BH,opt, which are somewhat skewed toward higher values.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: L5100 values vs. L 3.4 values. The blue-dotted line represents the best-fit correlation when α and β in Equation (4) are set as free parameters. The red-dashed line denotes the best-fit correlation when the slope term β is fixed to 1. Gray dashed–dotted and dashed–dot–dot–dotted lines show the best-fit correlations derived from the AGN templates of Richards et al. (2006) and Assef et al. (2010), respectively, where α and β are treated as free parameters.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) L bol,MIR/L bol,opt along with ﹩\mathrm{log}\left({L}_{{\rm{H}}\alpha }/{L}_{{\rm{H}}\beta }\right)﹩. Red circles represent the L bol,MIR/L bol,opt, and blue squares the dust extinction-corrected L bol,MIR/L bol,opt. (b) L bol,MIR/L bol,opt along with AGN power-law slope. The meanings of the red circles and blue squares are identical.