adsabs/AstroCLIMB huggingface dataset:
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The FPMA and FPMB background fit of NuSTAR observation 70660002004; this is a typical fit, and the results of the background fit for observation 70660002002 are similar. This fit was done with nuskybgd.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The raw 4–25 keV counts image of NuSTAR observation 70660002004. The background was extracted from the rectangular regions via nuproducts and fit with the nuskybgd code.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The temperature map of NuSTAR observation 70660002002. The annular regions and excluded point sources used in the spectral analysis are shown; the points were not excluded for the creation of the temperature map. The very cold area in the upper-right corner is due to the map going off the NuSTAR field of view.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The hydrostatic mass profiles corrected for nonthermal pressure support. The 1σ  posterior spread is propagated from the density and temperature posterior spreads found via MCMC (see Section 3.7). The radii r 2500 and r 500 are calculated with respect to the nonthermal-pressure-support-corrected Chandra data, and are found to be 589 ± 14 kpc and ∼1514 kpc, respectively. The dashed line shows the end of the largest extracted profile (XMM-Newton) at ∼837 kpc. In the top section, the total profiles are shown. In the bottom section, the ratios of the Chandra mass profile to the NuSTAR mass profile as well as the XMM-Newton mass profile to the NuSTAR mass profile are shown, with the NuSTAR mass profile as a reference.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The projected (blue) and 3D (red) models of the XMM-Newton temperature profile, fit with the T cool parameters free. The parameters for this fit are shown in Table 3. The 1σ posterior spread is found via Markov Chain Monte Carlo simulation as described in Section 3.7.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The projected (blue) and 3D (red) models of the NuSTAR temperature profile, fit with the T cool parameters free. The parameters for this fit are shown in Table 3. The 1σ posterior spread is found via Markov Chain Monte Carlo simulation as described in Section 3.7.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The projected (blue) and 3D (red) models of the Chandra temperature profile, fit with the T cool parameters free. The parameters for this fit are shown in Table 3. The 1σ posterior spread is found via Markov Chain Monte Carlo simulation as described in Section 3.7.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: Surface-brightness profile extracted from the mosaic Chandra image. The uncertainties on the extracted surface-brightness points are given as 3σ to make them more visible. The 1σ posterior spread shown is the Chandra model fit found via Markov Chain Monte Carlo simulation as described in Section 3.7.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The full (red) and hard (blue) band Chandra temperature fits. The solid blue points are the hard-band fits with the absorption (N H) fixed to the best-fit value found in the full-band fits. The dashed blue points are the hard-band fits when the absorption is left free to fit. The last annulus is not included for the hard-band fits because the signal-to-noise was low, which prevented the temperature from being constrained.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The observed temperature profiles from Chandra, NuSTAR, and XMM-Newton. The initial NuSTAR fit is in blue and the fit after running nucrossarf is in cyan.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: Results of the two-temperature-component simulations. The components were 4 and 5 keV, 4 and 6 keV, 4 and 7 keV, 5 and 6 keV, 5 and 7 keV, and 6 and 7 keV, and the normalizations were f min and ﹩(1-{f}_{\min })﹩, respectively. The fits are the result of the weighting equation with α = −0.35.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The double-β Chandra density profile fit. The parameters for this fit are shown in Table 4.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: The H I and CNM column densities (per unit velocity) in the outflow of M82. The teal curves show the CNM column density inferred from the [C II] spectrum (﹩{N}_{\mathrm{CNM}}^{[{\rm{C}}\,{\rm\small{II}}]}﹩) assuming collisions with only the atomic gas, T = 250 K, n = 100 cm−3, and C/H = 1.5 × 10−4. The thick magenta curves show N H I measured directly from the H I data. The thin magenta curves show the CNM column density inferred from the H I (﹩{N}_{\mathrm{CNM}}^{\mathrm{HI}}﹩) assuming f CNM = 0.5. The LFA pixels are oriented as in Figure 3, and the pixel numbers are given in the top left corner of each panel. The number in the top right corner of each panel is the ratio of the peaks of ﹩{N}_{\mathrm{CNM}}^{\mathrm{HI}}﹩ and ﹩{N}_{\mathrm{CNM}}^{[{\rm{C}}\,{\rm\small{II}}]}﹩ over the shaded portions of the profiles. The uncertainties come from a Monte Carlo analysis over the range of temperatures and densities considered.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: Similar to Figure 4, but showing the H2 column densities (per unit velocity) in the outflow of M82. The teal curves show the H2 column density inferred from the [C II] spectrum (﹩{N}_{{{\rm{H}}}_{2}}^{[{\rm{C}}\,{\rm\small{II}}]}﹩) assuming collisions with only H2, T = 250 K, n = 100 cm−3, and C/H2 = 3 × 10−4. The gray curves show the column density of H2 measured from the CO data (﹩{N}_{{{\rm{H}}}_{2}}^{\mathrm{CO}}﹩) assuming X CO = 0.5 × 1020 cm−2 (K km s−1)−1. The number in the top right corner of each panel is the ratio of the peaks of ﹩{N}_{{{\rm{H}}}_{2}}^{\mathrm{CO}}﹩ and ﹩{N}_{{{\rm{H}}}_{2}}^{[{\rm{C}}\,{\rm\small{II}}]}﹩ over the shaded portions of the profiles. The uncertainties come from a Monte Carlo analysis over the range of temperature and densities considered.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: A comparison of the [C II] and CO spectra in the disk of M82. The grayscale filled contours show the CO integrated intensity. The blue–green open contours show the [C II] integrated intensities (see the lines in the color bar). The black rectangle marks the fully sampled region of the [C II] map. The subplots show the spectra of the CO (gray) and [C II] (teal) extracted at the galaxy center (yellow), at the peak of the [C II] emission (cyan), and on the redshifted and blueshifted sides of the galaxy (red, blue). Both the CO and [C II] intensities are reported as main-beam brightness temperatures, and the data sets have been matched to the same spatial and spectral gridding and convolved to the CO beam size (22″). The black vertical lines in the panels show V sys  =  210 km s−1. Comparisons with H I are not possible to due strong absorption over this region (see Section 2.2.2).
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Distribution of the relevant global properties of our sample galaxies. Left: mass-concentration index (C 95) scatterplot of the sample (scatterplot), together with the marginal histograms of C 95 for the central and satellite subsamples, respectively. The dashed black lines in the main figure indicate the mass and C 95 intervals used for subsample definition. Middle: mass–color relation scatterplot of the whole sample (main figure), together with marginal histograms of (NUV-r) for the central and satellite subsamples. The dashed black line indicates the demarcation line of red quiescent dwarf and blue star-forming dwarf galaxies. The isodensity contours in the main figure enclose the central 34%, 68%, and 95% of the whole sample. Note that the demarcation between red and blue subsamples is chosen to approximately follow the upper limit of the 95% contour in the main figure. Right: histograms of the stellar mass of central and satellite galaxies.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: A PV diagram of the [C II] (filled colored contours) and CO (open grayscale contours) in the center of M82. This slice is extracted along the galaxy’s major axis and covers the entire fully sampled region of the [C II] map (3 × 1 kpc). The CO and [C II] data have the same beam size, pixel scale, and velocity resolution. The x-axis shows the offset along the galaxy’s major axis with respect to the center. The y-axis shows the velocity relative to V sys = 210 km s−1 (Krieger et al. 2021). In general, the kinematics of the CO and [C II] agree, though the [C II] velocity rises faster than the CO in the center.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: Left: the ratio of the [C II] to CO integrated intensities (in units of erg s−1 cm−2 sr−1 and K km s−1), in the same style as Figure 2. In the disk, the [C II] and CO data cubes, from which the integrated intensities are calculated, have the same beam size, pixel scale, and velocity resolution (see Section 4). Right: the estimated strength of the FUV radiation field based on the PDR model by Kaufman et al. (1999) using the ratios from the left plot and assuming a density of 104 cm−3.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: The CO and upGREAT [C II] luminosities in the disk (green–blue filled contours) and outflow (teal circles) of M82. The teal numbers indicate the pixel number of each outflow pointing. We compare our measurements to those from PACS (Contursi et al. 2013) in the grayscale contours. For all contours, the colors reflect the density of points. We also compare to integrated measurements from the xCOLD GASS survey of star-forming galaxies (red stars; Accurso et al. 2017).
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: HSC optical images of six dwarf galaxies randomly picked from our sample. The top (bottom) row shows galaxies at the low- (high-) redshift end of the sample. In each panel, the main figure is the i-band grayscale image, and the inset figure is the i-, r-, and g-band composite false-color red, green, and blue image. The i-band isophotal ellipses at 25 (green), 26 (blue), and 27 (red) mag arcsec−2 are overplotted on each main figure. The color images are created with the Lupton et al. (2004) method as implemented in astropy. visualization. make_lupton_rgb. The redshift and stellar mass of each galaxy are indicated at the lower left corner of each panel.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption:  H 0-estimates for the ZTF (top row) and Rubin Observatory (bottom row) observation scenarios for O4 (left column) and O5 BNS samples (right column). We show H 0-estimates from our GW simulations (in orange), EM simulations (in violet), and for the combined GW+EM results (in blue) in the top panels, whereas relative errors are shown in the bottom panels. We indicate the expected O4 and O5 detection rates in alignment with Table 5 as gray dashed line and show the the 90% credible interval as gray shaded regions. In the bottom panel, we contrast our results to the Planck measurement of the cosmic microwave background (Planck Collaboration et al. 2016; Planck, violet), to the Hubble measurement via type-Ia supernovae (Riess et al. 2016; SHOES, light blue), and to the H 0-measurement of superluminal motion of the jet in GW170817 (Hotokezaka et al. 2019; superluminal, gray). All uncertainties are reported at 90% credible interval.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: The plots at the top are BNS distributions of the missed and found injections (on the left, BNS light curves observed by ZTF, and the right one shows the same using Rubin Observatory), as a function of the peak r-band absolute magnitude and 2D probability enclosed. We encode in the color bar and the transparency of the points the 3D probability of finding the transient as measured by simulated injections. The 1D histograms are marginalized versions of the 2D scatter plot, with the detected set in green and missed set in red. The plots at the bottom are the same for the NSBH light curves. Those plots concern the run O4. In Appendix B.3, Figure 15 shows the same distribution for the run O5.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: This figure shows the simulated detections for O5. The upper panel shows the number of injections (CBCs from each population drawn from both distributions) in colored dots, and the bar chart represents the number of events passing the cutoff point. The bottom panel shows the percentage of detections relative to the number injections for the two distributions. The colored dots represent the percentages of each population that passed the S/N, while the blue and green lines with respectively 1.22% and 0.48% are successively percentages of detection of all the events (BNS + NSBH + BBH) of the PBD/GWTC-3 (GWTC-3) and LRR distributions injected in our simulation.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: 2D histograms of simulated BNS (left) and NSBH (right) light curves for O5. We show light curves in u, g, r, i, z, y, J, H bands in order to include all the bands used by surveys considered in this work (ZTF, Rubin, and Gemini). In each panel, we plot three dashed lines; on top the 10th percentile, at middle the 50th percentile, and on bottom the 90th percentile. The color bar shows the number of detections in the different bands.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Cumulative histogram of simulated GW skymaps for O4 that satisfy our triggering criteria as a function of the 90% credible region. With both Caltech and Partnership time spanning ∼50% of the night (corresponding to a maximum area of 800 deg2), we could fully probe the localization for nearly 40% of all events.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Here, we show all the O5 CBCs from all populations. On the left, the distribution of LRR; on the right, that of PBD/GWTC-3 (GWTC-3). The high panels are the mass distributions of the components of each CBC in the context of the detector, and the low panels are the primary mass distributions as a function of the collision distance. Mass and distance distributions are shown on a logarithmic scale. The color base shows the number of CBC events per pixel.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: 1D histograms of the peak magnitudes in the ZTF bands (in green) and the Rubin observatory bands (in red). On the left, we show the BNS peak mag in O4; on the right, the same plot for the run O5. See Figure 17, in Appendix B.2 for the peaks related to each band of each telescope.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Cumulative histograms of 100,000 realizations of the number of BNS and NSBH mergers predicted to be detected during LIGO-Virgo-KAGRA O4 and O5 within 400 Mpc based on the observing scenarios predictions in this paper. The mean number of expected detections is quoted for each merger type.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: 90% upper limit on the ﹩{M}_{\mathrm{ej}}^{\mathrm{wind}}﹩ measurements for the prompt collapse simulation set, where the ﹩{M}_{\mathrm{ej}}^{\mathrm{wind}}﹩ contribution is set to 0.
Paper: Spectra of V1405 Cas at the Very Beginning Indicate a Low-mass ONeMg White Dwarf Progenitor
Authors: Kenta Taguchi, Keiichi Maeda, Hiroyuki Maehara, Akito Tajitsu, Masayuki Yamanaka, Akira Arai, Keisuke Isogai, Masaaki Shibata, Yusuke Tampo, Naoto Kojiguchi, Daisaku Nogami, Taichi Kato
Figure caption: Spectra of V1405 Cas by the two low-dispersion grisms (VPH-blue and VPH-red, connected at 6050 Å) of KOOLS-IFU on t = +9.88, 23.77, 33.94, 71.79, and 81.90 hr, and by HDS (with the resolution artificially decreased to the KOOLS-IFU level, Section 3.1) on t = +53.53 hr. (a) An overall view of the normalized spectra. The lines labeled by the bold black font (He II, C III, and N III) are observed only at t = +9.88 hr. The Al II line labeled by the bold red font is one of the most striking lines discussed in Sections 3.3.3, 4, and 5. (b– e) Enlarged views of the spectra shown in panel (a).
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The contours of the ratio of our chemical timescales with an analytical timescale from Zahnle & Marley (2014) for N2, NH3, and HCN are shown in the log10 scale. The black solid line represents the T–P profile taken from Zahnle & Marley (2014) for effective temperature T eff = 600 K and g surface  =  103 cm s−2. The black dotted lines represent the contours of NH3/N2. The bottom right panel shows the ratio of the chemical timescale obtained in our study (t  q ) and from Zahnle & Marley (2014) (t  q   z ), for the thermal profile.