adsabs/AstroCLIMB huggingface dataset:
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The spectra of the afterglow obtained by Xinglong 2.16 m/BFOSC and NOT/ALFOSC, respectively. Top panel: the spectrum obtained by BFOSC. The gray line is the raw spectrum and the blue is smoothed for display purposes. Bottom panel: the spectrum obtained by ALFOSC. The gray line is the background sky spectrum and the red line is the raw spectrum of the burst. In the both panels, the identified metal absorption lines are indicated with vertical lines in the figure, and the possible lines at the left of Lyα are also marked. The gray vertical bands indicate the telluric features in both panels.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: Temporally symmetric model fit to GRB 220101A lightcurve. The left panel shows the 64 ms counts data (black) obtained by NaI detectors n6 and n7 of Fermi/GBM, the fit to the monotonic components (blue dashed line), the time-reversed model (red), the residual (blue), the time-reversed residual (green), the duration window (vertical dashed lines), and the time of reflection (vertical solid line). To display a clearer structure, the same GRB with a time resolution of 320 ms is shown in the right panel.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The multiband lightcurves of GRB 220101A. The detection points in the figure are in the AB system and have been corrected for Galactic extinction, which is E(B−V) = 0.05 (Schlafly & Finkbeiner 2011). The last i- and J-band points correspond to the HST F775W and F125W detections, respectively. The fits of different bands are represented by dashed lines of corresponding colors, and the fitting results are listed in Table 3.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The afterglow SED of GRB 220101A at 20 ks (Epoch 1, blue lines), 60 ks (Epoch 2, orange lines), 150 ks (Epoch 3, yellow lines), and 400 ks (Epoch 4, purple lines) from the optical to X-ray. The optical multiband data are listed in Table 4. The solid and dashed lines are the results of the single power law and the model fit for each epoch.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: “Kann plot” comparing a large sample of GRB optical afterglow lightcurves shifted in time and flux to a common redshift of z = 1 following Kann et al. (2010). The gray background are historical data of other GRB lightcurves. GRB 220101A is shown as a black solid line, which lies at the top of the distribution in terms of luminosity. The bursts with redshifts larger than 4 are colored in light blue.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: Posterior distribution and parameter constraints obtained using multiband afterglow modeling of GRB 220101A with afterglowpy. The median values with the 1σ error regions are also shown in the one-dimensional probability distribution.
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: Optical, near-infrared, and X-ray data of GRB 220101A along with the best-fit afterglow modeling. The shaded region is the 2σ error region. X-ray flux density is converted from 0.3 to 10 keV to 1 keV following Gehrels et al. (2008).
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The H I column density of z > 4 GRBs. The blue dashed line represents the average density of those with a redshift of between 4 and 5. The data points are collected from Thöne et al. (2013), Chornock et al. (2014), Laskar et al. (2018), and Saccardi et al. (2023).
Paper: Optical and Near-infrared Observations of the Distant but Bright “New Year’s Burst” GRB 220101A
Authors: Zi-Pei Zhu, Wei-Hua Lei, Daniele B. Malesani, Shao-Yu Fu, Dong-Jie Liu, Dong Xu, Paolo D'Avanzo, José Feliciano Agüí Fernández, Johan P. U. Fynbo, Xing Gao, Ana Nicuesa Guelbenzu, Shuai-Qing Jiang, David Alexander Kann, Sylvio Klose, Jin-Zhong Liu, Xing Liu, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Bringfried Stecklum, Christina Thöne, Joonas Kari Markku Viuho, Yi-Nan Zhu, Jin-Da Li, He Gao, Tian-Hua Lu, Shuo Xiao, Yuan-Chuan Zou, Li-Ping Xin, Jian-Yan Wei
Figure caption: The best fit of the Lyα break. The neutral hydrogen column density is ﹩\mathrm{log}\ ({\text{}}{N}_{\mathrm{HI}}/{{cm}}^{-2})=21.55\pm 0.08﹩ at a redshift z = 4.615.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: NIRSpec-IFU 1–5 μm spectra for each target extracted from a 1.″5 radius circular aperture. Each grating/filter combination has been color-coded, and 1σ error bars are indicated (darker gray), which are typically smaller than the line width. The envelopes (gray) show the 1σ variation of the spectral signal within the extraction aperture.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: 3.29 μm slices of the NIRSpec-IFU spectral–spatial data cubes. Indicated are the 1.″5 radius circular extraction apertures (black dashed) used in this work, the 0.″1 × 0.″1 pixel size, a 1″ scale bar, and the directions of north and east.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: VISTA image of part of NGC 2023. Image credits: ESO/J. Emerson/VISTA R. Gendler. Superimposed are telescope/instrument apertures for ISOCAM (pink), ISO-SWS (red), and Spitzer (blue slit) observations. The colored translucent overlay marks Spitzer-IRS spectral map observations, where each color represents one of four distinct emission zones identified through hierarchical clustering (see Boersma et al. 2016). The JWST aperture is shown and labeled in black.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: 1.6–1.7  μm region for each target, scaled and offset. The gray dashed lines bracket the nominal position of the v = 2–0 overtone of the 3.3 μm PAH band. It is noted that the triangle-like structure seen between ∼1.655 and 1.659 μm is the result of an incomplete removal of a data spike. See Section 4.1.2 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Hubble-ACS three-color composite image of IRAS 21282+5050, with F814W data shown in red, F606W data in blue, and an equal mixture of F814W and F606W data in green. Superimposed is the aperture from ISO-SWS (red) observations, and the apparent size of the nebula is indicated with the yellow dashed circle. The JWST apertures for the science target and separate dedicated background are shown and labeled in white, with the latter dashed.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Three-color composite infrared adaptive optics image of BD +303639 from the Gemini North 8 m telescope. The blue and red channels show narrowband H2 and Brγ emission, respectively. Image credits: Gemini Observatory, US National Science Foundation, and University of Hawaii Institute for Astronomy. Superimposed are apertures from ISOCAM (pink) and ISO-SWS (red) observations. The JWST aperture is shown and labeled in white.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: 3.2–3.6 μm region for each target, continuum subtracted, normalized to the peak strength of the 3.3 μm PAH feature, and offset. The gray dashed lines indicate the positions of the broad PAH-related features. See Section 4.1.1 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Three-color composite HST WFPC2 image of HD 44179, with the red channel taken from narrowband F631N data tracing [O I], the green channel from narrowband F588N data tracing He I, and the blue channel from medium Strömgren b-band F467M data. Superimposed is the aperture from ISO-SWS (red) observations. The JWST aperture is shown and labeled in white.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Three-color composite HST image of NGC 7027 with WFPC2 F55W data in red, F814W data in blue, and a combination of the two in green. Superimposed are apertures of ISOCAM (pink) and ISO-SWS (red) observations. The JWST aperture is shown and labeled in white.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: 4.3–4.8 μm region for each target, continuum subtracted and offset. Indicated are predicted regions where the aromatic and aliphatic CD stretches and the CN stretch in PAH nitriles fall (Bauschlicher et al. 1997; Hudgins et al. 2004; Allamandola et al. 2021; Esposito et al. 2023, in preparation). The gray dashed lines indicate their typical astronomical positions. *Range found for the aromatic CD stretch in pentacene. See Section 4.1.3 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Line analysis of M17-MC, given a line list of some 17,000 lines results in 1002 matches. Only lines with a signal-to-noise ratio of at least 2, a contrast of 5%, and an integrated intensity of at least 10−23 W cm−2 are shown. Each species/ionization state has been color-coded separately. The number of lines matched per species is provided in parentheses. Note that not all lines are matched, and there are those that are simultaneously matched by several species. Only 198 lines are spaced apart more than 5  ×  10−3 μm.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: 1–5 μm spectra of NGC 2023-PDR and NGC 1333-SVS3 indicating the PAH continuum (dark gray). The triangular shaped region below the 3.3/3.4 μm band complex (black line segments) designates emission associated with the 3 μm band complex. See Section 4.1.4 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Pure rotational (not extinction-corrected) H2 v = 0–0 population diagram analysis of the spectrum of M17-B-PDR. The propagated statistical uncertainties have been indicated. The blue line shows the best fit, with the derived parameters given, including their uncertainties. See Section 3.2.2 for details and Section 4.3 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Zoom-in and multicomponent decomposition of the 4.60–4.72 (aliphatic region; left) and 4.33–4.47 (aromatic region; right) μm spectra of M17-B-PDR. The properties of the component possibly attributable to deuterated PAHs (purple) are given. See Section 4.1.3 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Comparison of the observed 4.2 μm CO2-ice absorption (left) and CO rovibrational emission (right). See Sections 4.2 and 4.3 for discussions.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Warm, 258 K, CO gas detected in emission in the spectrum of IRAS 21282+5050-RIM-BKSUB. Note that the flat-appearing structure around 4.58 μm is due to a spike in the data being masked. See Section 4.3 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: Multicomponent fit of the CO2-ice absorption band in the spectrum of M17-B-PDR. The purple shaded area indicates the H2:CO2 (10:1) 10 K ice component. See Section 4.2 for a discussion.
Paper: JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look
Authors: C. Boersma, L. J. Allamandola, V. J. Esposito, A. Maragkoudakis, J. D. Bregman, P. Temi, T. J. Lee, R. C. Fortenberry, E. Peeters
Figure caption: The 2.3–3.1 μm spectrum of M17-B-PDR depicting a rich inventory of H I emission lines, notably the Pfund series, where each transition has been labeled separately.
Paper: A New Constraint on the Simulation of the Intergalactic Medium through the Evolution of the Neutral Hydrogen Fraction in the Epoch of Reionization
Authors: S. Mobina Hosseini, Bahareh Soleimanpour Salmasi, Seyed Sajad Tabasi, Javad T. Firouzjaee
Figure caption: This figure depicts the trend of the neutral hydrogen fraction variations in the IGM over time for all simulated models. This process of change is also pictured in the inset for the models that are more compatible with the IGM including f *7≤0.5 and f esc≤0.5. In order to provide a more comprehensive analysis of the process and provide a more robust comparison, the f *7, and f esc models were employed with 0, 0.1, 0.2, 0.3, 0.4, and 0.5 values. In the figure and the inset, observational data are represented as black points with their respective error bars according to Table 3.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: Top: posteriors on the relative lensing parameters for the GW191230–LGW200104 pair as determined by the GOLUM investigation. Bottom: the reconstructed posteriors for the source position and redshifted lens mass as calculated by the methodology presented in this work.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: Constructed candidate posteriors on the redshifted lens mass (left) and source position (right). The raw histogram of the samples is presented in black, the inferred posterior distribution using a KDE in blue, and the vertical red dotted line illustrates the true source position value. In this instance, the posteriors indicate a tight constraint with the true values of the parameters inside of the posterior and close to its mode—a successful recovery.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: Comparisons between the posterior on the relative magnification as determined by the GOLUM pipeline and the constructed posterior on the source position for the SIS model using the method presented in this work. The true value of these parameters is indicated by the red vertical dotted line. As can be seen, the constraint on the model parameter is dependent upon both the width and accuracy of the lensing observable constraint.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: The resulting value of the Bayes factors found by using every nth sample of the full set, scaled by the maximal value from the calculations to allow multiple events to be shown. As can be seen, a preliminary estimate of the Bayes factor, from applying the methodology using every 100th sample, would be robustly representative of the “final” estimate using all of the samples.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: Distribution of the log Bayes factors comparing the SIS and point-mass lensing models for the injection set. Shown in black is the raw histogram of these with the red overlay showing the inferred distribution from a kernel-density estimator. All events analyzed show a positive Bayes factor, which indicates that the SIS was correctly preferred in all cases.
Paper: Determination of Lens Mass Density Profile from Strongly Lensed Gravitational-wave Signals
Authors: Mick Wright, Justin Janquart, Martin Hendry
Figure caption: The results of the stability analysis for an event that demonstrates an initial deviation from the later stabilization value. Similarly to the main set, by approximately the inclusion of every 100th sample, the preliminary result would be representative of the final result.
Paper: A New Constraint on the Simulation of the Intergalactic Medium through the Evolution of the Neutral Hydrogen Fraction in the Epoch of Reionization
Authors: S. Mobina Hosseini, Bahareh Soleimanpour Salmasi, Seyed Sajad Tabasi, Javad T. Firouzjaee
Figure caption: Correlations between the z, T  K , T  S , S  α , x HI, and J 21 parameters are shown for four models, (a) f *7×0.1, (b) f *7×0.5, (c) f esc×0.1, and (d) f esc×0.5 in the pre-EoR.
Paper: A New Constraint on the Simulation of the Intergalactic Medium through the Evolution of the Neutral Hydrogen Fraction in the Epoch of Reionization
Authors: S. Mobina Hosseini, Bahareh Soleimanpour Salmasi, Seyed Sajad Tabasi, Javad T. Firouzjaee
Figure caption: Correlations between the z, T  K , T  S , S  α , x HI, and J 21 parameters are shown for four models, (a) f *7×0.1, (b) f *7×0.5, (c) f esc×0.1, and (d) f esc×0.5 in the EoR.