adsabs/AstroCLIMB huggingface dataset:
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The EX Lup spectrum dereddened with best-fit A  V  using a mixture of TWA 14 and TWA 25 spectra. The best-fit A  V  is 0.1 mag with synthetic spectrum made up of 97% TWA 14 and 3% TWA 25.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The same as Figure 21 but used an accretion model instead of assuming constant accretion fluxes. The best-fit A  V  and spectral type for EX Lup is 0.1 mag and M0.45. The parameters are adopted throughout the analysis of this paper.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The mass accretion rates of EX Lup between 1890 and 2022. DASCH B-band, AAVSO V-band, and ASAS-SN g- and V-band light curves are used to derive the accretion rates. Filled and hollow points are within and beyond the calibrated ranges of excess emission relations, respectively.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The rise and fall slopes in magnitudes per day, measured from the 10 bursts shown in Figure 14 (excluding the 1945 outburst), color coded by the accreted mass during the burst.
Paper: Steadiness of Coronal Heating
Authors: P. G. Judge
Figure caption: The mean of the time series is shown (top left) with the rms variations (top right) and their ratio (bottom left). The encircled region of enhanced variances is also indicated in Figure 5. The line plot shows the distribution of ﹩{\mathrm{log}}_{10}{\sigma }_{I}/{I}_{\mathrm{mean}}﹩, with the occurrences of larger variances magnified by a factor of 100 (red line). Only 21% of all the pixels have values of ﹩{\mathrm{log}}_{10}{\sigma }_{I}/{I}_{\mathrm{mean}}﹩ exceeding 0.1 in the logarithm, i.e., with values of σ  I  exceeding the mean by 26%.
Paper: Steadiness of Coronal Heating
Authors: P. G. Judge
Figure caption: Four images observed from SDO, including the 13.1, 17.1, and 9.4 nm AIA images that sample plasmas near 0.5, 1, and 6 MK, respectively, outside of flares. Arrows point to locations where the loop system discussed in the text is anchored. The close-up views in Figure 1 are centered near X = −180, Y = 250 in this figure. The encircled region in black shows a magnetic bipole emerging during the observations reported here, the white circle another smaller region of emerging flux.
Paper: Steadiness of Coronal Heating
Authors: P. G. Judge
Figure caption: Frequency-delimited variances (integrated power spectra) of the EUI time series are shown as in Figure 3.
Paper: Steadiness of Coronal Heating
Authors: P. G. Judge
Figure caption: The region of the Sun observed by the EUI instrument is shown as a full field of view (top left) and three close-up views. The bottom two panels show the two types of structure discussed in this paper; they are separated by just 60 s. The large loops are almost unchanged in 60 s. However, there is a region of dynamic evolution of EUV brightness in the upper half of these two bottom panels, possibly resulting from changes in magnetic topology. Intensities are on an arbitrary but identical scale for all panels. The squares show the areas shown in the right and bottom panels.
Paper: Steadiness of Coronal Heating
Authors: P. G. Judge
Figure caption: Close-ups of a region of quiet Sun are shown for the same frames shown in Figure 1.
Paper: EMRI + TDE = QPE: Periodic X-Ray Flares from Star–Disk Collisions in Galactic Nuclei
Authors: Itai Linial, Brian D. Metzger
Figure caption: Characteristic luminosity (top left; Equation (17)), duration (bottom left; Equation (16)), and spectral temperature (upper right; Equation (21)) of flares from disk–star collisions for a solar-mass EMRI for different SMBH masses and accretion rates as indicated. The bottom-right panel shows the ratio of the spectral temperature to that of the quiescent disk, T Q (Equation (5)), which may be taken as a metric of QPE observability. Solid and dotted lines show separately cases where the stellar radius is taken to be a solar radius or equal to Roche lobe radius for overflow onto the SMBH, respectively; a vertical dashed line corresponds to the minimum QPE period for a star with R ⋆ = R ⊙ (Equation (9)). Shown for comparison with black squares are the observed flare properties of long/short oscillating QPE (Table 1); the thickness assigned to the boxes are somewhat arbitrary and not to meant to encompass observational uncertainties or time-variation. We assume α = 0.1 and R isco = 4R g for the viscosity and inner radius, respectively, of the quiescent disk.
Paper: EMRI + TDE = QPE: Periodic X-Ray Flares from Star–Disk Collisions in Galactic Nuclei
Authors: Itai Linial, Brian D. Metzger
Figure caption: Characteristic flare luminosity (top left; Equation (A3)), duration (top right; Equation (A2)), and spectral temperature (bottom; Equation (21)) from the collision of the secondary SMBH of mass m • with the accretion disk of the primary SMBH of mass M • = 108 M ⊙ (blue lines) or M • = 1010 M ⊙ (red lines) at a radius r 0 = 100R g(10R g); these roughly correspond to the pericenter distance of the hypothesized {e ≈ 0.7, P orb ≈ 9 yr } orbit of the SMBH binary candidate OJ 287. Shown for comparison in the gray shaded regions are the ranges of observed properties of previous optical/UV flares from OJ 287 (e.g., Valtonen et al. 2008, 2012). We assume α = 0.1 and R isco = 4R g for the viscosity and inner radius, respectively, of the quiescent disk. Although the low-M • models can fit the durations and spectral temperature of the OJ 287 flares, they are generally not sufficiently luminous.
Paper: Observation of Alfvén Ion Cyclotron Waves in ICME Magnetic Clouds at 1 au
Authors: Omkar Dhamane, Vinit Pawaskar, Anil Raghav, Zubair Shaikh, Raffaella D'Amicis, Kalpesh Ghag, Kishor Kumbhar, Daniele Telloni, Georgios Nicolaou, Prathmesh Tari, Robert Wicks, Utsav Panchal, Bhagyashri Sathe, Prachi Pathare
Figure caption: Time-frequency distribution of correlation coefficients between V  Ai  and V  i  for the entire event. Solar wind speed and magnetic field are shown in the fourth panel. Temperature anisotropy and θ VB are plotted in the last panel. WIND satellite 3 s observations from MFI and 3DP, in addition to the Solar Wind Experiment (92 s; Ogilvie et al. 1995) for temperature anisotropy are utilized for the analysis.
Paper: Observation of Alfvén Ion Cyclotron Waves in ICME Magnetic Clouds at 1 au
Authors: Omkar Dhamane, Vinit Pawaskar, Anil Raghav, Zubair Shaikh, Raffaella D'Amicis, Kalpesh Ghag, Kishor Kumbhar, Daniele Telloni, Georgios Nicolaou, Prathmesh Tari, Robert Wicks, Utsav Panchal, Bhagyashri Sathe, Prachi Pathare
Figure caption: The interplanetary parameters correspond to the ICME’s transit (shaded area) on 2000 July 31, shown in the figure. The panels from top to bottom represent total IMF (B mag in nanotesla), the absolute value of IMF fluctuation, i.e., ﹩\delta {B}_{i}=\tfrac{{B}_{i+1}-{B}_{i-1}}{2}﹩; IMF vector components, i.e., (B comp); azimuth (ϕ), and elevation (θ) angle; proton density (N  p  in centimeters cubed); plasma velocity (V  p  in kilometers per second); temperature (T  p  in kelvins); and plasma beta (β).
Paper: Observation of Alfvén Ion Cyclotron Waves in ICME Magnetic Clouds at 1 au
Authors: Omkar Dhamane, Vinit Pawaskar, Anil Raghav, Zubair Shaikh, Raffaella D'Amicis, Kalpesh Ghag, Kishor Kumbhar, Daniele Telloni, Georgios Nicolaou, Prathmesh Tari, Robert Wicks, Utsav Panchal, Bhagyashri Sathe, Prachi Pathare
Figure caption: Panel (a) shows the spectral analysis of trace of magnetic field (PSD(B  x )+PSD(B  y )+PSD(B  z )). Top part of panel (b) demonstrates spectral analysis e + and e −; in addition, bottom part shows the variation of σ  c  in the frequency domain. In the top part of panel (c), PSD of e  v  and e  b  is plotted along with that in the bottom part, where variation of σ  R  is shown.
Paper: Observation of Alfvén Ion Cyclotron Waves in ICME Magnetic Clouds at 1 au
Authors: Omkar Dhamane, Vinit Pawaskar, Anil Raghav, Zubair Shaikh, Raffaella D'Amicis, Kalpesh Ghag, Kishor Kumbhar, Daniele Telloni, Georgios Nicolaou, Prathmesh Tari, Robert Wicks, Utsav Panchal, Bhagyashri Sathe, Prachi Pathare
Figure caption: The normalized magnetic helicity spectrum, σ  m , is represented in color within this composite figure. It is plotted at various evenly spaced angles, θ VB, and combined to create the final visualization. Each vertical slice in the figure corresponds to the spectrum σ  m  at a specific look angle, θ VB, relative to the local mean magnetic field direction.
Paper: EMRI + TDE = QPE: Periodic X-Ray Flares from Star–Disk Collisions in Galactic Nuclei
Authors: Itai Linial, Brian D. Metzger
Figure caption: Schematic view of our model. A star orbits an SMBH that is accreting matter through a thin disk of scale height h at a rate ﹩\dot{m}﹩. Due to the inclined orbital plane, the star impacts the disk twice per orbit, carving a hole through the disk and ejecting an optically thick cloud of material expanding above and below the disk plane. As the ejecta expands and cools, photons begin to diffuse out, and the light curve peaks once the optical depth drops below c/v ej, where v ej ∼ v K is the ejecta velocity imparted by the colliding star. The inner regions of the disk dominate the soft quiescent emission seen between the collision-powered flares.
Paper: Observation of Alfvén Ion Cyclotron Waves in ICME Magnetic Clouds at 1 au
Authors: Omkar Dhamane, Vinit Pawaskar, Anil Raghav, Zubair Shaikh, Raffaella D'Amicis, Kalpesh Ghag, Kishor Kumbhar, Daniele Telloni, Georgios Nicolaou, Prathmesh Tari, Robert Wicks, Utsav Panchal, Bhagyashri Sathe, Prachi Pathare
Figure caption: PSD of B mag and σ  m  for MC is plotted. The 11 Hz magnetic field data of the WIND spacecraft instruments are used for estimation.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: Comparing the profile model of Equation (2) (left) to the NFW profile (right). The gray dots are random points generated based on these two density profile models for halo mass M = 12. The light blue circles indicate the virial radius of the halo mass M = 12. The blue dashed–dotted curves illustrate the circular velocity ﹩{v}_{c}^{2}﹩. The green dotted curves show the mass interior to r, i.e., M(<r). The yellow dashed curves display the gravitational potential ϕ. The red solid curves showcase the f cs. The amplitudes of the curves are rescaled in order to be visible in the same figure. The coordinate axes indicate the radial distances from the halo center and are rescaled to r/(10R vir).
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The top panel shows the correlation functions. The blue filled circles (for which the error bars are small enough to be unnoticeable except on very small scales) are the measured correlation function using the real-space Cartesian coordinates of the DARK SAGE galaxies. The red solid curve is the model correlation function fit to the measurements using our new halo density profile for galaxies. The pink dashed–dotted curve is the model correlation function calculated using the NFW profile and the yellow dots of the bottom panel. In the bottom panel, the green line is the HOD inferred from the fitted correlation function using our new profile model and the yellow dots are the measured HOD (the error bars are tiny). So our fitting method combined with the new profile model does an excellent job of recovering the true HOD from fitting only the correlation function. The fit results of the HOD parameters are displayed in Figure 10 of Appendix B.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: NIRCam color-composite image of the RX J2129.4+0005 lensing cluster (R: F356W+F444W, G: F200W+F277W, and B: F115W+F150W). The two z ≈ 8.15 galaxies are indicated by red circles; insets show the positions of the NIRSpec MSA slits. The upper inset shows the photometry of RX2129–ID11002 at z spec = 8.16 (R.A.(J2000.0) = 21:29:39.904, decl.(J2000.0) = 00:05:58.83) and the lower inset shows RX2129–ID11022 at z spec = 8.15 (R.A.(J2000.0) = 21:29:36.080, decl.(J2000.0) = 00:04:56.53). We do not expect these galaxies to be multiply imaged; the lensing magnifications are presented in Table 2.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The top panels show the HOD of satellite galaxies measured from the SDSS galaxies. The bottom panel shows the galaxy two-point correlation functions ξ  gg (r). The blue dots are the measurements from SDSS galaxies. The red solid curve is the model ξ  gg (r) inferred from the measured HOD in the top panel and the halo density profile for galaxies (Equations (2), (5), and (6)). The pink dashed–dotted curve is the model ξ  gg (r) inferred from the measured HOD in the top panel and the NFW profile.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The fit results of the HOD parameters. The histograms display the distribution of our Markov Chain Monte Carlo samples. The shaded areas in the 1D histograms indicate the 68% confidence level, while the 2D contours indicate the 1, 1.5, 2, and 2.5σ regions.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: Comparing the f cs and f  ss  of SDSS galaxies to those of DARK SAGE and the NFW profile, in an example halo mass bin M = 14.15.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The PDF (the radial distribution) of satellite galaxy pairs f  ss  for two example halo mass bins. The yellow and green filled circles are the measurements from DARK SAGE for halo mass bins centered on M = 12.68, 14.86 respectively. The solid curves show the model calculated from Equation (9), using the mass-dependent parameter values for α (Equation (5)) and β (Equation (6)). The dashed curves showcase the NFW profile for these masses. All of them are normalized to integrate to one in the interval x ∈ [0, 1].
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The Fourier transformation for the galaxy number density profile of halos, in two example halo mass bins. The pink and blue filled circles are the measurements from DARK SAGE for halo mass bins centered on M = 12.80, 13.87, respectively. The solid curves are the model calculated from Equations (11) to (2), using the mass-dependent parameter values for α (Equation (5)) and β (Equation (6)).The dashed curves showcase the NFW profiles for these masses.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: Mass–metallicity relation at z ≈ 8. Colored data points show the distribution of the measured masses and metallicities for the sources in our sample of z ≈ 8 galaxies. The solid red line and the shaded pink region respectively show the best-fit z ≈ 8 mass–metallicity relation and its 1σ uncertainty, if the mass–metallicity relation is fitted with a free slope. The solid orange line and the shaded orange region respectively show the best-fit z ≈ 8 mass–metallicity relation and its 1σ uncertainty, as inferred by fixing the slope to the empirical value at lower redshifts, γ g = 0.3. The solid black line show the predicted mass–metallicity relation at z = 8 based on FIRE simulations (see Ma et al. 2016), showing remarkable agreement with our findings. For comparison, we also show the best-fit mass–metallicity relation at lower redshifts. The green, blue, and dark purple lines respectively show the best-fit mass–metallicity relation at z ≈ 3.3, 2.3, and 0 inferred by Sanders et al. (2021) based on data from the MOSDEF survey. The light purple line shows the best-fit line at z ≈ 0 from Curti et al. (2020). There is a significant ∼0.9 dex evolution in the normalization of the mass–metallicity relation from z ≈ 8 to the local universe; on average galaxies are 8 times more metal enriched at z ≈ 0 compared to z ≈ 8. The evolution persists by 0.5 and 0.4 dex with respect to the average galaxies at z ≈ 2.3 and z ≈ 3.3, respectively. The dashed section of each solid line indicates extrapolation beyond the investigated stellar mass range of the corresponding study.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: [O III] 5007 Å/Hβ line flux ratio plotted against the [O II] 3727, 3729 Å/Hβ line flux ratio for six galaxies at z spec ≈ 8 (large colored data points), as inferred from the JWST NIRSpec observations of the RX2129 and SMACS0723 lensing clusters. The small dark-green data points show the measurements for the EELGs at z spec ≲ 1 from the zCOSMOS survey. The dashed red contours indicate the weighted 1σ and 2σ confidence intervals for the z ≈ 8 sample; since the weighted confidence intervals for this sample are dominated by the tight constraints on the SMACS0723–ID6355 galaxy we also show the unweighted 1σ and 2σ confidence intervals as the shaded red region. The shaded green region indicates the 1σ and 2σ confidence interval for the z spec ≲ 1 EELGs sample. Moreover, we show the blueberry (small purple data points) and green pea (small light-green data points) galaxies from Yang et al. (2017a, 2017b), confirming their remarkable strong emission line similarities (see also Figure 7) to the emission-line-detected galaxies at z ≈ 8; this is especially the case for the blueberry galaxies, almost all of which lie within the 2σ credible interval of the z ≈ 8 galaxies.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: Strong line metallicity indicator comparison. This Figure shows O32 ([O III] 5007 Å/[O II] 3727, 3729 Å) plotted against R23 − 0.08 × O32 (R23 × Hβ = [O II] 3727, 3729 Å + [O III] 4959 Å + [O III] 5007 Å) for the six galaxies at z ≈ 8 with available NIRSpec strong emission line measurements (large colored data points). The shaded red region (dashed red line) show the unweighted (weighted) 1σ and 2σ confidence intervals of the z ≈ 8 sample. For comparison we show the zCOSMOS EELGs at z spec ≲ 1 (small dark-green data points) as well as their weighted 1σ and 2σ confidence intervals (the shaded green region). We also show the blueberry (small purple data points) and green pea (small light-green data points) galaxies from Yang et al. (2017a, 2017b). Both here and in Figure 6, blueberry galaxies (and green peas to a lesser degree) occupy a region similar to the z ≈ 8 emission-line-detected galaxies, which indicates that they have remarkably similar strong emission line features and metallicities. However, as shown in Figure 11, the addition of the stellar mass parameter can distinguish these local-analog candidates from z ≈ 8 emission line galaxies in the context of the mass–metallicity relation.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the RX2129–ID11002 galaxy. The top panel shows the observed (orange circles) and best-fit photometry (green squares) as well as the best-fit spectra (green line). The six smaller panels on the bottom right show PDFs of the stellar population synthesis parameters. The dotted lines show the assumed priors. The stellar mass here refers to the total stellar mass formed before correcting for dead stars. The bottom left panel shows the SFH modeled nonparametrically with five temporal bins. All parameters are corrected for lensing magnification.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: Emission lines fits (using pPXF) to the NIRSpec 1D spectrum of the RX2129–ID11002 (see Figure 2) galaxy at z spec = 8.16. The dashed orange line shows the stellar continuum fit and the dashed blue line shows the Gaussian fits to the emission lines; the solid purple line shows the combined continuum plus emission lines fit. The line widths are fixed to the spectral resolution of the NIRSpec prism at the observed wavelength. The measured emission line fluxes are reported in Table 2.