adsabs/AstroCLIMB huggingface dataset:
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: Left: the luminosity-weighted age gradient as a function of M * for SFGs with R e > R e,median. The mean age gradient is marked by the red dashed line. Large symbols show the median ∇age values of each stellar mass bin, with a bin size of ΔM * = 0.2  dex. The shaded region indicates the region of 16–84 percentile. Right: similar to the left panel, but for SFGs with R e < R e,median. The red region indicates the region of 16–84 percentile for the R e > R e,median subsample.
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: The T-Type distribution for ∇age > 0 and ∇age < −0.25 subsamples. We show the results in two stellar mass bins, with log (M */M ⊙) < 10.3 (left panel) and log (M */M ⊙) > 10.3 (right panel). The p-value of the Kolmogorov–Smirnov test is also marked.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Spectra around the resonance line K I λ7699. The stars shown have effective temperatures within 32 K of each other. The dotted (solid) spectra are uncorrected (corrected) for telluric O2 absorption.
Paper: Local Star-forming Galaxies Build Up Central Mass Concentration Most Actively near M ∗ = 1010 M ⊙ 
Authors: Zhizheng Pan, Xianzhong Zheng, Xu Kong
Figure caption: Similar to Figure 2, with the SFG sample of 0.02 < z < 0.05.
Paper:  r-process Abundance Patterns in the Globular Cluster M92
Authors: Evan N. Kirby, Alexander P. Ji, Mikhail Kovalev
Figure caption: Syntheses of the CH feature (red) compared to the observed spectra (black). These spectra sample three different stellar luminosities in M92.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Stacked radial peculiar velocities and relative number density in and around superclusters. The x-axis denotes the distance from the supercluster center in units of r  s  (half the size of a supercluster). (a) Two-dimensional histogram of the mock halos in and around superclusters. N denotes the number of halos in each grid. The region (r/r  s  ≲ 1 and v pec,h  ≲ 0) contains most of the member halos of a supercluster. (b) Mean (blue line) values of the radial peculiar velocity component as a function of scaled distance. The shaded blue region shows the standard deviation (1σ) of the radial peculiar velocity component. The red line shows the relative number density of halos as a function of scaled radius. This relative number density is calculated by dividing the average number density ρ  N  (of all stacked superclusters) at a scaled radius by the total number density 〈ρ  N 〉 of halos within a sphere of radius ∼8 × r  s .
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Radial peculiar velocities of the member clusters of all (stacked) superclusters as a function of their comoving distance from the supercluster center. The black line represents a peculiar velocity of 0 km s−1, and the red line represents all the peculiar velocities equal and opposite to the Hubble flow as seen from the center. The three regions, divided by red and black lines, are Hubble Decoupled: members that have decoupled from the Hubble flow; Supercluster Influence: members that have not decoupled from the Hubble flow, but have slowed down in their Hubble expansion; and Outside Influence: member clusters that have their velocities greater than the Hubble flow and therefore have gravitational influence from regions outside of the supercluster.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: (a) Number of candidate superclusters for different linking lengths l 0 for WHL and the mocks. The curves peak at 19.22 Mpc and 19.88 Mpc for WHL and the mocks, respectively, and are represented by dotted lines. (b) Density contrast of the mock superclusters as a function of size. The blue dots represent the mock superclusters, the red line is a linear fit to the data points on the log–log plot, and the shaded red region denotes the associated errors in the fit. The slope of the fitted line is given at the top right corner of the plot. The black line and the shaded black region denote the corresponding fit and the associated errors of WHL superclusters presented in Figure 6(c).
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: The most massive supercluster in the mock. The “∗” symbol indicates the center of mass of the supercluster. Member clusters are represented by circles and their colors indicate the masses M 200c . The red arrows show the supercluster-centric peculiar velocity components (radial peculiar velocities) of the member clusters, with arrow lengths proportional to the radial peculiar velocities. Here, an arrow with a length of 1 Mpc corresponds to 60 km s−1.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Sky plane distribution of the five most massive superclusters identified in our supercluster catalog.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Optical images of the most massive member clusters in each of the top five superclusters in Table 2. Abell 2631 is actually the most massive cluster of SCl 4 (the Saraswati supercluster). The images are extracted from the DESI Legacy Imaging Surveys (DR9).
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Distributions of the size, mass, density contrast, and the number of member clusters of the superclusters in WHL and HR4 within 0.05 ≤ z ≤ 0.366.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Time evolutions of the height (a) and velocity (b) of the HC. The pink dashed line delineates the result of curve fitting using Equation (1). The brown and orange dotted lines represent the onset time of the fast rise and the start time of the flare, respectively.
Paper: A Lack of 9 s Periodicity in the Follow-up NuSTAR Observation of LS 5039
Authors: Oleg Kargaltsev, Jeremy Hare, Igor Volkov, Alexander Lange
Figure caption: Left and right panels show the total (from the entire observation) Fourier power spectrum (top) and the dynamic Fourier power spectrum (bottom; zoomed on the region near the 9 s candidate signal) from the 2016 and 2022 NuSTAR observations, respectively. The detailed description of the left panels in Figure 1, given in V+21, also applies to the right panels (since the length of the observation and the number of photons from the target are very similar for both observations) and, hence, we do not reproduce it here.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: (a) Outer (blue “+” symbols) and inner (cyan “+” symbols) boundaries of the HC. The elliptic torus is superposed with red dots. The black dashed line denotes the elliptic axis. Two green solid lines are used to separate the flare from the HC. (b) AIA 131 Å image at 10:36:45 UT superposed with the elliptic torus (magenta dots). (c) A 3D visualization of the elliptic torus with Matlab.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Running-difference images of the CME observed by LASCO/C2 during 10:48–11:12 UT (top panels) and by STB/COR1 during 10:56–11:06 UT (bottom panels). The white arrows point to the CME and CME-driven shock.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Reconstructed DEM profiles of eight regions within the HC (a)–(h) and four regions within the flare site (i)–(l). The red solid lines represent the best-fitted DEM curves from the observed values. The black dashed lines represent the DEM curves from 100 MC simulations. The values of 〈T〉 and ﹩\mathrm{log}\ {\mathrm{EM}}_{{\rm{c}}}﹩ are labeled.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Full-disk STB/EUVI 195 Å image at 11:16:23 UT (a) and 171 Å image at 12:14:53 UT (b). The orange dotted–dashed lines represent the longitude line passing through AR 11302. The short magenta lines represent the PIL. The arrows point to the PFLs of the X1.4 flare.
Paper: A Lack of 9 s Periodicity in the Follow-up NuSTAR Observation of LS 5039
Authors: Oleg Kargaltsev, Jeremy Hare, Igor Volkov, Alexander Lange
Figure caption: Folded (with a 3.90608 days orbital period) binary lightcurves from the 2016 and 2022 NuSTAR observations in 3–79 keV range.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Radio dynamic spectra recorded by e-Callisto/BLEN7M (a) and Ondrejov/PHOENIX3 (b) during the flare impulsive phase. The yellow arrows point to the type III and IVm bursts.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Distribution of merger fraction in the A O − M 20 diagram. The black density map is the number density of the subsample. In each panel, the contours from outer to inner represent the merger fraction, which is 2, 3, and 4 times the average value in each subsample masked by red numbers. The solid blue line is the merger candidate selection criterion in each subsample. The peak of the merger fraction at A O = 1.2, M 20 = − 1.3 in the low-z subsample and A O = 1.4, M 20 = − 1.3 in the high-z subsample.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: The top three panels show the comparison between spec-z and the most reliable phot-z in the COSMOS2020/CLASSIC sample, while the bottom three panels show the phot-z in our work. Galaxies with ∣z phot − z spec∣ > 0.15(1 + z spec) are considered outliers (Hildebrandt et al. 2012). Phot-z error is defined by Hoaglin et al. (1983) and denoted by σ NMAD.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Distributions of the merger and nonmerger samples in the nonparametric parameter space. The green and magenta contours refer to nonmerger and merger samples. The histograms are the normalized number density of these parameters. Relative separation is given above each histogram.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Distribution of stellar masses and redshifts of the galaxies with i < 25.5 at 0.2 ≤ z best ≤ 1 in the COSMOS HST/ACS F814W imaging survey covered area. The blue and red lines are the empirical stellar mass completeness for the star-forming and quiescent galaxy sample computed by Weaver et al. (2022). Our sample is the galaxies above the magenta dotted line.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Example images of merging galaxies. From the left two panels to the right two panels show the merging galaxies with tidal tails, double nuclei, merger remnants, close pairs, and pairs with disturbed morphologies respectively. The redshift and stellar mass are labeled on each image. The length of the white line in each image is 1′′.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Example images in the A O − M 20 diagram. The blue (red) contours are SFGs (QGs) number density distribution.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Distribution of SFGs, QGs, and mergers in the A O − M 20 diagram.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Overview of the HH 80/81 giant outflow in an Hα mosaic from the APO 3.5 m telescope obtained with the 30 Å bandwidth filter. This image has had a large-scale intensity gradient removed. The blue oval shows the location of IRAS 18162-2018 (GGD 27) and the approximate orientation of the radio jet emerging from this source. Yellow lines surrounding GGD 27 show the approximate location and spatial extent of the outflow cavity walls as traced in Spitzer 8 and 24 μm images. Dashed red circles mark the locations of various shocks and radio features. A blue circle near the top marks the location of radio source 34 at the suspected end of the radio jet. The magenta oval marks the location of the infrared dark cloud (IRDC) discussed in the text. A red “X” symbol near the source region marks the B2/B3 star located at the center of the circular near-IR H2 bubble discussed in the text. The small, unlabeled, dashed circle near the bottom along the radio jet axis marks the location of a diffuse Hα knot which is also shown in Figure 13.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Merger fraction and merger rate as a function of the redshift. The filled markers represent major mergers selected by morphological methods (Lotz et al. 2008b; Conselice et al. 2009; Jogee et al. 2009; López-Sanjuan et al. 2009), whereas the unfilled markers denote massive close pairs (Bundy et al. 2009; de Ravel et al. 2009; Lackner et al. 2014; Man et al. 2016). The blue-filled and black-unfilled markers refer to the visual and pair samples in our work, respectively. The blue and black dashed lines represent the best-fit relation of our visual and pair samples, respectively. The error bars of our markers are statistical errors.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Star formation rate excess as a function of the stellar mass in mergers. Magenta and green markers indicate the visual and pair samples, respectively. The left panel represents the low-z subsample, while the right panel represents the high-z subsample.
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Merger fraction in the Gini − M 20 diagram. Contours from outer to inner represent the merger fraction, which is higher than 2,3 times the mean value in the parent sample.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The full field observed in 2018 with HST showing HH 80/81 in [S II].
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: AGN fractions excess in different stellar mass bins for the visual merger sample and the pair sample. The shadow region in each panel refers to the massive bins (log(M */M ⊙) >10.5).
Paper: Revisiting Galaxy Evolution in Morphology in the Cosmic Evolution Survey Field (COSMOS-ReGEM). I. Merging Galaxies
Authors: Jian Ren, Nan Li, F. S. Liu, Qifan Cui, Mingxiang Fu, Xian Zhong Zheng
Figure caption: Comparison of the nonparametric morphological parameters in the F814W and the F125W images.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The full field observed in 2018 with HST showing HH 80/81 [O III].
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: A continuum-subtracted 2.12 μm H2 image showing the immediate vicinity of IRAS 18162-2048. The dashed, red ovals mark H2 emitting MHOs with the designations given in Mohan et al. (2023). Small, red circles show the locations of the cluster of sources detected by Busquet et al. (2019). Dashed blue and red arrows show the orientations of multiple outflows emerging from the core containing IRAS 18162-2048 (Fernández-López et al. 2013).
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: A continuum-subtracted 2.12 μm H2 image showing the IRAS 18162-2048 field and the field located to the northeast containing HH 80N A (HH80N). Small, red circles show the locations of the cluster of sources detected by Busquet et al. (2019). Dashed blue and red arrows show the orientations of multiple molecular outflows emerging from the core containing IRAS 18162-2048 identified by Fernández-López et al. (2013). Small, dashed, red circles in the southern field show some of the MHOs in the southern field. The yellow lines mark the locations of the mid-IR cavity walls as in Figure 1. The larger, dashed, red, circles in the northern field are the HH objects marked in Figure 1.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The giant Hα bow shock inflated by the radio jet south–southwest of GGD 27 in a continuum-subtracted image formed by subtracting a scaled SDSS i band image from the narrowband Hα image. The Hα image was obtained using the 78 Å bandpass filter. Dashed arrow marks the orientation and extrapolated location of the radio jet from IRAS 18162-2018. Dashed circles mark the locations of compact Hα knots close to the radio jet axis. See text for details.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: A continuum-subtracted 2.12 μm H2 image of the region north of IRAS 18162-2048 containing HH 80N. Dashed cyan lines show the outline of the cavity walls seen in the Spitzer 24 μm images. The yellow lines mark the approximate location of the outflow cavity walls centered on the IRAS source as seen in the Spitzer 8 and 24 μm images. These are also as shown in Figure 1.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The immediate vicinity of IRAS 18162-2048 in a continuum-subtracted [Fe II] image. The red circle marks the location of IRAS 18162-2048.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: An Hα image taken with the 30 Å filter showing the HH objects in the counterflow direction north of IRAS 18162-2048 The magenta oval marks the location of the IRDC north of HH 80N A (previously HH 80N) which is discussed in the text.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 80 in [O III]. Red shows 1995 epoch Hα observed with WFC2's WF channel. Cyan shows the 2018 epoch [O III].
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 81 in [O III]. Red shows 1995 epoch Hα observed with WFC2's PC channel. Cyan shows the 2018 epoch [O III].
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 80 in [S II]. Red shows 1995 epoch Hα observed with WFC2's WF channel. Cyan shows the 2018 epoch [S II].
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 (left) and background-subtracted, exposure-corrected (right) 0.8–2 keV counts images of the Chandra observations. A spectrum was extracted from each of the annuli shown; these spectra were fit to get the observed temperature profile. The excluded regions are the point sources manually selected from a 0.5–4.0 keV image. The radii of the annuli are 30″, 68″, 101″, 152″, 228″, 342″, and 513″.
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 (left) and background-subtracted, exposure-corrected (right) 0.4–7.2 keV counts images of the combined MOS1/MOS2/PN XMM-Newton observation. A spectrum was extracted from each of the annuli shown; these spectra were fit to get the observed temperature profile. The excluded regions are the same as used for Chandra and NuSTAR.
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 exposure-corrected, background-subtracted 4–25 keV image of NuSTAR observation 70660002004. A spectrum was extracted from each of the annuli shown, excluding the point sources. The annuli have the same radii as shown in Figure 1, though the outermost annulus is not included. These spectra were fit to get the observed temperature profile.