adsabs/AstroCLIMB huggingface dataset:
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 model b18.3-mean. 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 (contributions from all the tracer particles are counted by taking the masses as a weight), 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: 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), for the models b18.3-mean (top), b18.3-sphel (middle), and b18.3-sphel-pure (bottom). The top panel is the same as the lower right panel in Figure 14.
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: 1D calculation results with the angle-averaged profiles for the model b18.3-high (Ono et al. 2020) with the parameters, f h = 10−2, f d = 10−2, and t s = 500 days (upper panel), and f h = 5 × 10−3, f d = 10−2, and t s = 500 days (lower panel). The time evolution of the total amounts of CO and SiO, and the seed atoms, carbon, oxygen, and silicon, are shown. The points are the estimations for CO and SiO in the previous studies; for the details, see the caption of Figure 14.
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 16 but for the parameters of f h = 10−4, f d = 1.0, and t s = 500 days (left panel), and f h = 10−4, f d = 10−2, and t s = 500 days (right panel).
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 12 but for silicon monoxide (SiO).
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 18 but for silicon monoxide (SiO).
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 evolutions of the mass fractions (not the total amounts) of molecules and several seed atoms (left panels) and the gas temperatures (right panels). From top to bottom, the results for the models b18.3-zp, b18.3-zn, and b18.3-yp are shown, respectively. In the right panels, colors denote the initial positions of the particles.
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 results of the 1D calculation with the effective energy deposition rate in Equation (B4) with the angle-averaged profiles for the model b18.3-high (Ono et al. 2020) with the parameters, f h = 5 × 10−3, f d = 1.0, and t s = 500 days (top panels, b18.3-mean-nledep) and the ones of the corresponding counterpart model without the nonlocal energy deposition, i.e., the model b18.3-mean (bottom panels, same as the top panels in Figure 20) for comparison. Left panels: time evolution of the total amounts of molecules and several seed atoms 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). Right panels: time evolution of the gas temperatures of the tracer particles; the colors denote the initial positions of the particles. As a reference, power-law evolutions of the powers of −1 and −2 are shown on the right panel.
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: Radial distributions of the number densities of CO and SiO (solid lines) at the end of the calculation for the models b18.3-zp, b18.3-zn, b18.3-yp, n16.3-zp, n16.3-zn, and n16.3-yp. For reference, approximated number densities of CO and SiO (dashed lines, C × O and Si × O, respectively) are also plotted. Here, C × O (Si × O) denotes ﹩\sqrt{N({\rm{C}})\times N({\rm{O}})}﹩ (﹩\sqrt{N(\mathrm{Si})\times N({\rm{O}})}﹩), where N(C), N(O), and N(Si) are the number densities of carbon, oxygen, and silicon atoms, respectively, for the case with no chemical evolution, i.e., the case that each tracer particle keeps the initial mass fractions of the species. From top to bottom, the models for the directions, +Z, −Z, and +Y, are shown, respectively. The left panels (right panels) are for the models based on the binary merger progenitor model b18.3 (single-star progenitor model n16.3).
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 20 but for the models n16.3-mean (top panels), n16.3-sphel (middle panels), and n16.3-sphel-pure (bottom panels).
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 24 but for the models n16.3-zp, n16.3-zn, and n16.3-yp.
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: Rate coefficients of the electron impact excitation/deexcitation of vibrational levels, q  ij , in Equation (23) as a function of temperature obtained based on Poparić et al. (2008). For example, the coefficient corresponding to the transition of the state i = 0, to j = 1 is denoted as “01” in the legend.
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: Radial profiles of the mass fractions of the molecules and several seed atoms for the models b18.3-zp (top), b18.3-zn (middle), and b18.3-yp (bottom). Left panels: the profiles at approximately 200 days. Right panels: the profiles at the end of the calculation.
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 26 but for the models n16.3-zp (top), n16.3-zn (middle), and n16.3-yp (bottom).
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 20 but for the models n16.3-mean (top), n16.3-sphel (middle), and n16.3-sphel-pure (bottom).
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 results of the maximum-likelihood analysis for NGC 253. The top panel shows the likelihood contours drawn at 0.5σ intervals, with the abscissa giving the galaxy’s true distance modulus, and the ordinate showing the number of PNe within 2.5 mag of M* normalized to the amount of galactic bolometric light contained in the two MUSE data cubes. The lower panel marginalizes over this variable. The distribution is quite wide, due to the dearth of PNe in the top ∼1 mag of the luminosity 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 cumulative luminosity function for PNe in NGC 253. The dark line represents the observed data; the curve is Equation (2) shifted to the most likely apparent distance modulus. The dashed line shows the location where incompleteness and the PNLF’s star formation dip cause the curve to overpredict the number of PNe. 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: Blue and red regions of the spectrum of the bright, highly extincted planetary PN3 found in pointing P1 of NGC 253. The y-axis is in units of 10−20  erg  cm−2 s−1 Å−1. The extreme Hα/Hβ ratio indicates an extinction of A 5007 ∼ 2.1 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: The top panel shows the results of the maximum-likelihood analysis for NGC 1326. 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 red contours, shown at 0.5σ intervals, illustrate the likelihoods when PN1 is included in the sample; the likelihood that PN1 is a superposition of two bright [O III] sources is reflected in the distorted probability contours at the ∼3σ level. The black contours display the same information when PN1 is excluded. The bottom panel marginalizes these data 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 observed PNLF of NGC 1351 binned into 0.2 mag intervals. The open circles beyond m 5007 ≳ 28.0 show data beyond the completeness limit; the open circle at m 5007 ∼ 26.8 represents PN1, an object that is 0.2 mag more luminous than the next brightest source. The error bars illustrate 1σ confidence intervals (see Gehrels 1986). The red curve illustrates the most likely fit to Equation (2) when PN1 is included in the sample; the black curve shows the fit when PN1 is excluded. The difference between the values is 0.16 mag. A K-S test excludes PN1 from the sample with 93% confidence.
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 1326 binned into 0.2 mag intervals. The open circles beyond m 5007 ∼ 27.8 represent data beyond the completeness limit; the bright open circle shows PN1. The error bars represent each bin’s 1σ confidence intervals (Gehrels 1986). The red curve illustrates the most likely fit to Equation (2) when PN1 is included in the sample; the black curve shows the fit when PN1 is excluded. The difference between the solutions is 0.17 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: The top panel shows the results of the maximum-likelihood analysis for NGC 1351. 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 red contours, shown at 0.5σ intervals, illustrate the likelihoods when PN1 is included in the sample; the black contours display the same information when PN1 is excluded. The bottom panel marginalizes these data 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: Top: the observed PNLF of NGC 1052 binned into 0.2 mag intervals, with error bars displaying 1σ confidence intervals (see Gehrels 1986). Open circles represent data beyond the completeness limit of the survey. The top panel shows the PNLF where the PN emission has been deblended from the DIG using the methods described in Paper I; the lower panel shows the same function when the sky estimates are based on simple aperture photometry. The curves show the best-fit PNLF: without deblending, the most likely apparent distance modulus is 0.25 mag smaller.
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 small region of the MUSE data cube for NGC 1351, showing one wavelength slice centered on [O III] λ5007 at the redshift of the galaxy. Note that PN1 is blended with PN16. The overluminous nature of PN1 may be due to an imperfect deblending of the two sources.
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 results of the maximum-likelihood solution for NGC 1052's distance modulus. The top panel shows the likelihood contours (drawn at 0.5σ intervals), with the abscissa giving the galaxy’s true distance modulus and the ordinate showing the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The lower 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 observed PNLF for NGC 1433 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 bottom panel displays the full data set, along with three curves which all assume an apparent distance of (m − M) = 31.36, but with different amounts of an additional photometric error added in quadrature (0.0 mag for the black curve, 0.1 mag for red, and 0.2 mag for green). The top panel shows the data when the three fields with poorly known aperture corrections are excluded. The magnitude distribution is a much better match to Equation (2) and implies a most likely apparent distance modulus of (m − M) = 31.45.
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 1404 binned into 0.2 mag intervals. The open circles denote data beyond the completeness limit; the error bars represent 1σ confidence intervals (see Gehrels 1986). The black curve shows the most likely fit to Equation (2). Note that the process of binning makes the brightest PNe appear exceptional; in fact, it is only 0.04 mag more luminous than the second brightest object.
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 1433. Left: thumbnail off-band and difference images derived from the MUSE data cubes. Our PNe candidates are highlighted in blue, while emission-line interlopers are shown in red. Note that the numbering of markers is assigned to the individual pointings P1…P9, not to the final sample of the galaxy as a whole. Right: a broadband image of the galaxy with the MUSE fields outlined in white. (Credit: CGS). A high-resolution image of the off-band and difference images is available in 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 upper panel shows the results of the maximum-likelihood solution for NGC 1404. 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, and the contours are drawn at 0.5σ intervals. The lower panel marginalizes over the PN/light 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 upper panel shows the results of the maximum-likelihood solution for NGC 1419. 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, and the contours are drawn at 0.5σ intervals. The lower panel marginalizes over the PN per unit light 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: A comparison between our PN photometry for NGC 1404 and that of Spriggs et al. (2020); the error bars for the latter are estimated from the inverse of the quoted peak amplitude to residual-noise level ratio (A/rN). The standard deviation of the distribution is 0.13 mag, and the mean offset between the two data sets (excluding the two outliers) is 0.006 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: The cumulative luminosity function for PNe in NGC 1419. The dark line represents the observed data; the curve is Equation (2) shifted to the most likely apparent distance modulus of (m − M)0 = 31.42. The dashed line shows where incompleteness begins to affect the 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 top panel shows the results of the maximum-likelihood solution for the Antennae galaxy. 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 red contours are for the analysis that includes PN1, while the black contours show the likelihoods without the object. As the marginalization in the bottom panels shows, the difference in the solutions is ∼0.05 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: The top panel shows the results of the maximum-likelihood solution for NGC 4418. 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. There is a slight possibility that the galaxy’s brightest PN candidate is the superposition of two sources; this is reflected in the bump in the outermost likelihood contour.
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 4472 binned into 0.2 mag intervals. Open circles denote data beyond the completeness limit; the error bars illustrate the uncertainties of small number counting statistics (Gehrels 1986). The curve shows Equation (2) shifted by the best-fit apparent distance modulus of (m − M) = 30.91.
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 4365 binned into 0.2 mag intervals. Open circles denote data beyond the completeness limit; the error bars reflect the small number counting statistics (Gehrels 1986). The black curve shows Equation (2) shifted by the best-fit apparent distance modulus of (m − M) = 31.61.