adsabs/AstroCLIMB huggingface dataset:
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: Comparison of the BH mass estimates for sources where both Hα and Hβ FWHMs are simultaneously available (left), for sources where both Hβ and Mg II FWHMs are simultaneously available (middle), and for sources where both Mg II and C IV are simultaneously available in a spectrum (right). In each panel, the dotted black line represents the 1-to-1 line shown for reference. The sources from the SDSS DR14 QSO sample are shown using contours where the Hβ-, Mg II-, and C IV-based BH masses are reported (no Hα). For the SDSS sample, we filter the sources based on the fiducial L bol and M BH with the QUAL flags = 0. The largest contour represents 67% of the total number of the SDSS AGNs.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption:  M BH distributions from the cleaned SDSS DR14 QSO sample (Rakshit et al. 2020). The Hβ- (red), Mg II- (green), and C IV-based (blue) masses are shown in this histogram. The respective median values are shown using dashed lines of identical colors, while the shaded regions mark regions bounded by the 16th and 84th percentiles for the respective distributions.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: AGN luminosity at 5100 Å (left panel), 3000 Å (middle panel), and 1350 Å (right panel) derived from the OGLE photometry as a function of redshift. The respective marginal distributions are shown per panel. The medians are marked with dashed lines, and the shaded regions mark the region between 16th and 84th percentiles of the distributions in each of the marginal distributions.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: Binned spectra for the sources highlighted in the right panel of Figure 7, corresponding to three R Fe II regimes—low (in red, 0.146 ± 0.005), medium (in green, 0.998 ± 0.009), and high (in blue, 2.1068 ± 0.018). The shaded region shows the Fe II range (4434–4684 Å), and the central wavelength for the Hβ is marked using the dotted line.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: Mass–radius relationship of our short-period CBs. The red solid line represents the best-fitting result as R  s /R  p  = q 0.435. The black solid line represents the fitting result as R  s /R  p  = q 0.38 for the upper bound, and the magenta solid line represents the fitting result as R  s /R  p  = q 0.48 for the lower bound. The upper bound region is the deep fill-out CBs and the lower bound region is the shallow fill-out CBs.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Similar to Figure 10, but for the MILES spectra. It is worth mentioning that the fine-tuned UaRA-net applied here uses the NGSL spectra rather than the MILES spectra. The red line denotes the systematic difference between the MILES spectra and NGSL spectra yielded by their common stars. The blue and red lines match well.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals for the predicted NGSL SEDs with the fine-tuned UaRA-net. The blue lines denote the medians and the standard deviations of relative residuals as a function of wavelength. Top panel: training set. Bottom panel: testing set.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: The RMSAE of the predicted NGSL SEDs as a function of A  V  for the training (top panel) and testing (bottom panel) set with the fine-tuned UaRA-net.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals for the predicted NGSL SEDs when directly applying the pretrained UaRA-net. The spectra are ranked by the T eff from 5000 to 9750 K.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: The SEDs from the UaRA-net and observations and their relative residuals for the training and testing sets at different S/Ns. A total of six representative stars of different spectral types are plotted.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals for the training (top panel) and testing (bottom panel) sets of the predicted NGSL SEDs with the fine-tuned UaRA-net.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals for the training (top panel) and testing (bottom panel) set of the MILES results at R = 2000 using GPR.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals of the GPR training (top panel) and testing (bottom panel) set for MILES.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Similar to Figure 12, but for NGSL.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Relative residuals between the generated NGSL-based spectra and the MILES spectra of the common sources.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: One-zone calculation results for three sets of the parameters, f h = 10−4, f d = 5 × 10−2, and t s = 200 days (top panels); f h = 5 × 10−4, f d = 10−2, and t s = 200 days (middle panels); f h = 10−3, f d = 10−2, and t s = 200 days (bottom panels). Left panels: time evolution of the amounts of CO and SiO and the seed atoms, carbon, oxygen, and silicon, compared with the estimations (including theoretical calculations) for CO and SiO in previous studies, LD92 (Liu et al. 1992), LD94 (Liu & Dalgarno 1994), LD95 (Liu & Dalgarno 1995), ALMA (Matsuura et al. 2017), and L+20 (Liljegren et al. 2020). The time evolution of gas temperature is also plotted. Right panels: time evolution of the fluxes for CO vibrational bands, Δv = 1 (fundamental), Δv = 2 (first overtone), …, Δv = 6, compared with the observed light curves for Δv = 1 (BD93; W+93; Bouchet & Danziger 1993; Wooden et al. 1993, respectively), and Δv = 2 (M+89, 93; BD93; Meikle et al. 1989, 1993; Bouchet & Danziger 1993, respectively).
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Initial radial profiles along the specific directions, +Z (top), −Z (middle), and +Y (bottom), for the model b18.3-high at the age of 19.0 hr after the explosion. Mass fractions of species as a function of the radius (left) and the density, temperature, and radial velocity as a function of radius (right).
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Same as Figure 7 but for the model n16.3-high and at the age of 22.3 hr after the explosion.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Same as Figure 3 but for the purely spherical case for the models b18.3-high (top) and n16.3-high (bottom), and the ages are 17.0 and 20.0 hr after the explosion for the former and latter models, respectively.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Contributing chemical reactions for the formation (left) and destruction (right) of CO in which carbon monoxide (CO) is directly involved as a function of time (after 30 days) for the one-zone calculation of the case with f h = 5 × 10−4, f d = 10−2, and t s = 200 days. The code inside the parentheses left side of each reaction denotes the corresponding reaction type listed in Table 2. Colors denote the relative contribution of each reaction, which is proportional to the reaction flow F  i  (D  i ) in Equation (1), normalized as the maximum F  i  (D  i ) among CO formation (destruction) reactions at each time to be unity. For neutral–neutral (NN) reactions, net contributions are counted by subtracting the reaction flow of the corresponding inverse reaction. Reactions are picked up if the relative contribution once becomes greater than 10−3.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Same as Figure 3 but for the spherical explosion case for the models b18.3-high (top) and n16.3-high (bottom), and the ages are 21.4 and 24.0 hr after the explosion for the former and latter models, respectively.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: One-zone calculation results for the case of f h = 10−4, f d = 5 × 10−2, and t s = 200 days. Top panel: the time evolution of the population of CO vibrational levels X  i  and the mean escape probability ﹩\overline{\beta }﹩. Bottom panel: the time evolution of the gas density; for reference, a power-law evolution with the power of −3 is also shown. For the details, see the text.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Time evolution of the amounts of CO and SiO and the seed atoms, carbon, oxygen, and silicon, compared with the estimations (points) for CO and SiO in previous studies (for the explanation of the points, see the caption of Figure 9). Left panel: f h = 10−2, f d = 10−2, and t s = 200 days. Right panel: f h = 5 × 10−4, f d = 1.0, and t s = 200 days.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Isosurfaces of the mass fractions of elements, 56Ni (red), 28Si (green), 16O (blue), and 12C (cyan), in the 3D hydrodynamical models (Ono et al. 2020) b18.3-high (left) and n16.3-high (right) with arrows denoting the +Z-, −Z-, and +Y-directions. The snapshots for the models b18.3-high and n16.3-high are at 19.0 and 22.3 hr after the explosion, respectively. Isosurfaces corresponding to 10% (lighter color) and 70% (darker color) of the maximum value for each element are shown.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: One-zone calculation results with f h = 5 × 10−4, and f d = 10−2 for the comparison of different t s values. From top to bottom, the results for t s = 200, 300, 500, and ∞ days are shown, respectively. Left panels: time evolution of the population of vibrational levels of CO, the gas temperature, and the mean escape probability ﹩\overline{\beta }﹩. Right panels: time evolution of the fluxes of CO vibrational bands, Δv = 1 (fundamental), Δv = 2 (first overtone), …, Δv = 6, compared with the observed light curves for Δv = 1 (BD93; W+93; Bouchet & Danziger 1993; Wooden et al. 1993, respectively), and Δv = 2 (M+89, 93; BD93; Meikle et al. 1989, 1993; Bouchet & Danziger 1993, respectively). The top right panel is the same as the middle right panel in Figure 9.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: The reduction factors f red as a function of time for the parameter values of t s = 200, 300, and 500 days.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood solution for NGC 1399's distance modulus. The abscissa is the galaxy’s true distance modulus, the ordinate is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ intervals. The bottom panel marginalizes over α 2.5.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood analysis for NGC 1366. The abscissa is the galaxy’s true distance modulus, the ordinate is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ levels. The bottom panel marginalizes these data over the PN per luminosity variable.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF of NGC 1399 binned into 0.2 mag intervals. The open circles show data beyond the completeness limit; the error bars represent 1σ confidence intervals (see Gehrels 1986). The black curve illustrates the most likely fit to Equation (2).
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The cumulative luminosity function for PNe in NGC 1366. The dark line represents the observed data; the curve is Equation (2) shifted to the most likely apparent distance modulus of (m − M)0 = 31.39. The dashed line shows the location where the incompleteness begins to affect the PN detections. Data brighter than this are consistent with being drawn from the empirical function.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF of NGC 1385 binned into 0.2 mag intervals. The error bars represent 1σ confidence intervals (see Gehrels 1986); the open circles show data beyond the completeness limit. The black curve illustrates the most likely fit to Equation (2).
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood analysis for NGC 1385. The contours are drawn at 0.5σ intervals. The abscissa is the galaxy’s true distance modulus; the ordinate is the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The bottom panel marginalizes over the latter variable.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top three panels show our maximum-likelihood solution for NGC 1433. The abscissa is the galaxy’s true distance modulus, while the ordinate for the top three panels is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ intervals. Three different solutions are shown: one where the errors are solely those reported by the PN photometry, and two others where we assume the existence of additional random uncertainties due to poor background subtraction and our inability to accurately measure each cube’s aperture correction. The bottom panel marginalizes these solutions over α 2.5. Note how the galaxy’s inferred distance depends on the photometric precision.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood analysis for NGC 1512. The abscissa is the galaxy’s true distance modulus, the ordinate is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ intervals. The bottom panel marginalizes over α 2.5. Note the bimodal solution: there is a non-negligible probability that PN1 is a superposition of two objects.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF for NGC 1512 binned into 0.2 mag intervals. Open circles denote data beyond the completeness limit; the error bars are from small number counting statistics (Gehrels 1986). The red curve shows the most likely fit to Equation (2) when PN1 is included in the analysis; the black curve shows the solution when PN1 is assumed to be made up of a superposition of two sources (or is excluded from the analysis altogether).
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: NGC 2207/IC 2163. Left: thumbnail off-band and difference images derived from the MUSE data cubes. The majority of pointlike [O III] sources are interloping objects (red markers); there are only three PN candidates (blue markers) present in the field. Right: a broadband image with the MUSE pointings outlined in white. (Credit: ESO). A high-resolution image of the off-band and difference images is available online.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF for the Antennae galaxy binned into 0.2 mag intervals. Open circles denote data beyond the completeness limit; the error bars are from small number counting statistics (Gehrels 1986). The red curve shows the best fit to Equation (2) when PN1 is included in the analysis; the black curve shows the best fit when this one object is excluded. The two distance moduli differ by 0.048 mag.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: A possible overluminous PN in NGC 3501. The PN may be a superposition of two [O III] emission-line sources with a separation of 0.″4, but the poor (1.″51) image quality precludes a definitive statement.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The combined PNLF from the 14 galaxies listed in Table 11. The PNe’s absolute magnitudes have been computed using each system’s most likely apparent distance modulus. The dashed line shows our assumed empirical PNLF (Equation (2)); the solid curve gives the expected PNLF when accounting for the formal errors of each galaxy’s distance determination. (The effect of field-to-field aperture correction errors for those galaxies observed with multiple MUSE pointings is not included in the analysis.)