adsabs/AstroCLIMB huggingface dataset:
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Comparison of scale height results from the 1D and 2D methods. Left: the average h  z  from the 1D sech box model and h  z  from the GALFIT EdgeOnDisk model. Right: thick disk h  z  from the 1D sech2 model and h  z  from the 2D EdgeOnDisk model.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Top: histogram of resulting uncertainties from the 2D EdgeOnDisk model. Bottom: histogram of resulting uncertainties from the 1D sech2 model.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Data, model, and residual images of our sample from 2D fits using GALFIT EdgeOnDisk model. Images are in units of counts with linear color distributions.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: (Continued).
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Radial profile of the scale height for our sample. Radii are normalized to the optical radius R 25.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Radial profile of the scale height for our sample. Error bars represent statistical uncertainties from fits.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Histogram of ﹩{V}_{\max }﹩ for galaxies showing the presence of a thick disk (red) and those that do not possess such a component (blue).
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Successful vertical fits of our sample. Square points represent 3.6 μm data. The red solid line is the total best-fit model composed of two distinct components: the thin disk component (dashed blue line) and the thick disk component (dotted–dashed green line). See Section 3.2 for details.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Distribution of h  z  ratio.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Comparison of scale height results from 3D and 2D methods.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Ratio of the scale heights at R 25 and at R = 0 against the morphological type T. Error bars are uncertainties arising from statistical errors.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Left: single-component scale heights as a function of the face-on central surface brightness. Right: single-component radial-to-vertical scale length ratio against the face-on central surface brightness. Our results are represented by the dark circles. Square and triangle symbols are, respectively, the B- and K s-band data from A. V. Zasov & D. V. Bizyaev (2003). Dashed dark lines indicate linear fits from these data points.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Scale height of the thin disk as a function of the maximum velocity ﹩{V}_{\max }﹩. Red solid circles and blue diamonds represent galaxies with and without a thick disk, respectively. Note that both dust-obscured and unobscured data from YD6 have been plotted. Left: correlation obtained from inclination-corrected scale heights. Right: relationship for the uncorrected scale heights.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Partial correlations between scale heights and galaxy properties with control parameters (color bars). h  R  represents the radial scale length, R 25 the apparent radius, ﹩{V}_{\max }﹩ the maximum velocity, M ⋆ the current stellar mass, and T the morphological type. The red bar shows the original correlation coefficient. Left: correlations for single-component scale height. Middle: relationships for thin disk scale height. Right: thick disk scale height and galaxy properties.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Relationship between scale height h  z  and scale length h  R  for single-component fit results. The observed tight correlation can be used as an empirical relation for estimating scale height.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Left: correlation between single-component scale height h  z  and the uncorrected apparent radius R 25. Right: oblateness and R 25.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: The disk oblateness against the scale length from our results (closed circles) and data from M. A. Bershady et al. (2010) for Sb–Sdm galaxies in I, H, and K bands (open triangles). The left panel shows uncorrected data; the right panel has data points corrected for inclination.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Left: thin disk scale height as a function of the apparent radius R 25. Right: relationship between thick disk scale height and R 25.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Scale height ratio and maximum velocity.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Photon count spectra from two NICER observations that demonstrate a change in the X-ray soft excess occurring independently from the hard X-ray power-law state. The total data (source and background) are shown as gray points, with the best-fit model from Section 3.4 in black. The data-to-model ratios for each bin are shown as gray points below. The source model (dashed lines) contains a power-law continuum (purple), a blackbody soft excess (blue), and a narrow Gaussian representing the Fe Kα line (pink). The background model (dotted lines) contains a Gaussian optical noise peak (red), the non-X-ray background (brown), and the sky X-ray background (yellow). Left: this observation was taken on MJD 58400 when the Swift UVW2 flux was near minimum (ObsID 1100020169). The X-ray power law has flux ﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{PL}})=-10.347\pm 0.004﹩ (all fluxes are reported in units of erg cm−2 s−1) and Γ = 2.11 ± 0.01. The soft excess flux is ﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{SE}})=-12.364\pm 0.008﹩. Right: an observation from MJD 59060 taken near Swift UVW2 maximum (ObsID 3100020364), with ﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{PL}})=-10.200\pm 0.003﹩ and Γ = 2.23 ± 0.01. The soft excess flux is log(ΦSE) = −11.260±0.008.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Left: light curves of the best-fit flux values of the fixed Γ = 2.15 model in Section 3.2 for each NICER spectrum, in descending order: total source flux (light purple), power-law continuum flux (﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{PL}})﹩; dark purple), blackbody soft excess flux (﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{SE}})﹩; dark blue), and Swift UVW2 flux density (ϕ  ν,UVW2; light blue). Near UVW2 minimum (MJD 58300–58500), fixing Γ produces model fluxes higher than those observed in the soft X-rays, causing the soft excess flux to be pegged at the minimum value of 10−16 erg cm−2 s−1 (see Table 1). Right: cross-correlation functions relative to the UVW2 reference band (solid line), with histograms representing the probability distributions of the peak (purple) and centroid (gray) lag values.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Corner plot showing the parameter distributions for the model in Table 1 applied to the observation on MJD 58256. Both the power-law index Γ and the blackbody soft excess flux ﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{SE}})﹩ are free parameters and are fit using the Markov Chain Monte Carlo method with 100,000 steps and an initial burn-in of 20,000 steps. Dashed lines on the histograms represent the lower 1σ confidence interval, the median, and the upper 1σ interval. Contours represent 0.5σ, 1σ, 1.5σ, and 2σ. A clear degeneracy between Γ and ﹩\mathrm{log}({{\rm{\Phi }}}_{\mathrm{SE}})﹩ is evident in the central bottom panel, given the shape of the distribution.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Top: light curve of Fairall 9 using NICER XTI (purple) and Swift XRT (orange) from 0.3 to 8 keV. The axes are rescaled to account for NICER’s 20× greater sensitivity than Swift. NICER source count rates are measured by subtracting the contribution of the best-fitting SCORPEON background model. Bottom: hardness ratio of NICER observations, which demonstrates variability in the observed spectral shape. The H band covers 1.5–8 keV, while the S band covers 0.3–1.5 keV.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Changes in the best-fit χ 2 value of the “UVW2-linked soft excess” model, created by shifting the soft excess light curve by lag (τ; left) and UVW2/soft excess flux scaling factor (A; right). The χ 2 statistic is summed across all 383 epochs for each value of τ and A. Purple lines highlight the ΔΣ(χ 2) = 1, and intersections with the black line represent the limits of the 68% confidence interval (1σ) for τ and A.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Left: light curves showing slow variability in the X-ray power-law flux (top; purple) and UVW2 flux density (bottom; blue), adapted from Figure 4 and smoothed using a rolling boxcar average at each epoch with a width of 30 days. Right: cross-correlation functions calculated using UVW2 as the reference band, with histograms representing the peak (colored) and centroid (gray) probability distributions. The peak X-ray/UV correlation is R peak = 0.66 at a lag of ﹩\tau =-{3.4}_{-6.0}^{+8.8}﹩ days.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Top: energy contributions from the fast variability components of the X-ray (purple) and UVW2 (blue) light curves in Figure 6, which are detrended using a rolling boxcar average with a width of t = 2–200 days for each epoch. Energies are calculated as a percentage of the total AGN power based on F var (Equation 2) and the SED modeling results of S. Hagen & C. Done (2023). Middle: R peak between the fast variability components of the X-ray and UV light curves after detrending with a common boxcar width t. Bottom: R peak between the slow variability components of the X-ray and UV light curves, produced using a boxcar average with full width t.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Same as Figure 7 but for slow variability isolated with a boxcar width of 150 days. The X-ray/UV correlation is very high (R peak = 0.92) and peaks at a lag of ﹩\tau =-{17.8}_{-1.0}^{+1.4}﹩ days, indicating that the X-rays lead the UV on long timescales. The ICCFs are extremely flat as a consequence of the broad boxcar width.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Schematic of the accretion flow of Fairall 9. The thermal accretion disk is shown in a gradient from red to light blue. The peak UVW2 disk emission in the direction of the observer is represented by a blue arrow originating at R UVW2. The warm corona (dark blue) layers the thermal disk, extending to R WC. A dark blue arrow represents emission from the warm corona, plus X-rays from the hot corona (purple) that are gravitationally redshifted and reflected off of the inner disk as soft X-rays.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Same as Figure 4 but for the best-fitting UVW2-linked soft excess model in Section 3.4. The central panel shows the power-law index Γ, which represents the spectral shape of the hot X-ray corona and was a fixed parameter in the light curves of Figure 4. Here, the soft excess flux curve (fourth panel) is determined by Equation (1), with best-fitting values for A and τ shown in Figure 5, and is held fixed during spectral fitting.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Light curves of count rate (top panel), power-law flux (middle panel), and power-law index (bottom panel) measured for each epoch of observation with Swift XRT (orange squares) and NICER XTI (purple circles). The data reduction process is described in Appendix B. A significant offset in the measurement of Γ by the two instruments is visible in the bottom panel, indicated by the black lines, which represent the sample median for NICER (dashed) and Swift (solid).
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Same as Figure 13 but for simulated spectra using the FAKEIT command in XSPEC corresponding to the best-fit model from each NICER epoch, as described in Appendix B. Swift XRT data are shown as orange squares, and NICER XTI data are shown as purple circles. The black lines in the bottom panel show the median values of Γ for NICER (dashed) and Swift (solid). Despite the differing response matrices for each instrument, the measured Γ values agree, in contrast to the real data in Figure 13.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: Same as Figure 7 but for the fast variability component of the light curves, calculated by subtracting a 30 day wide boxcar average from the original light curves in Figure 4. The X-ray/UV correlation is not statistically significant, peaking at R peak = 0.27 with a lag of τ = −1.0 ± 0.8 days.
Paper: Connecting the X-Ray/UV Variability of Fairall 9 with NICER: A Possible Warm Corona
Authors: Ethan R. Partington, Edward M. Cackett, Rick Edelson, Keith Horne, Jonathan Gelbord, Erin Kara, Christian Malacaria, Jake A. Miller, James F. Steiner, Andrea Sanna
Figure caption: The difference (Δ) between the 0.3 and 8 keV background rate measured by SCORPEON and 3C50, plotted vs. the Δ in background-subtracted source count rate (top panel; light purple), power-law spectral index Γ (middle panel; dark purple), and ﹩{\chi }_{\nu }^{2}﹩ (bottom panel; black). The Pearson correlation coefficient R is listed for each panel, demonstrating a lack of a significant relationship between the parameters.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) Magnitude vs. size for sources detected and measured in the i + r coadd. The points shown in red are stars matched with the Gaia EDR3 catalog. All sources inside the black box are rejected from the weak lensing analysis pipeline. So are the sources above the horizontal yellow line (15th magnitude) to account for the brighter-fatter effect. Sources to the right of the vertical yellow line are rejected to avoid blended sources and artifacts. Sources to the left of the curved yellow line are also rejected since these are three standard deviations smaller than the median PSF. (b) The photon counts vs. size graph for the i + r coadded image simulated using PhoSim for the first case of γ 1 = 0.1. The points in the red box are used for PSF interpolation. The points inside the black box are not used for the shear analysis. The condition for the red box is 3.3 < size < 3.8 pixels and 500 < counts < 105. For the black box the conditions are 2.5 < size < 4.5 pixels and 102 < counts < 106.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) The points show the ﹩{\sigma }_{{xx}}^{2}﹩ of stars in the i + r coadded image. The red curve shows the best-fit Gaussian obtained with a width half the value of P 84 − P 16, where P  i  represents the ith percentile value. The fits are reasonably good though not perfect. (b) and (c) shows similar graphs for ﹩{\sigma }_{{yy}}^{2}﹩ and ﹩{\sigma }_{{xy}}^{2}﹩. The widths of the Gaussians are 0.37, 0.27, and 0.08, respectively. (d) The points show the ﹩{\sigma }_{{xx}}^{2}﹩ of stars in the i + r coadded image simulated using PhoSim for the first case, i.e., γ 1 = 0.1. The red curve shows the best-fit Gaussian for each case. (e) and (f) show similar graphs for ﹩{\sigma }_{{yy}}^{2}﹩ and ﹩{\sigma }_{{xy}}^{2}﹩. The widths of the Gaussians are 0.18, 0.22, and 0.06, respectively.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) On the left an example of background from a typical chip is shown. On the right, the background from chips with correlated noise is shown. Correlated noise gives rise to spurious sources, especially at the faint end. (b) An example of crosstalk caused by very bright sources. This image shows a portion of the OTA. QuickReduce is unable to get rid of all cases of crosstalk arising from extremely bright sources. Coadding reduces them to a nondetectable level. However, some of the severe cases are apparent in the coadd. The vertical line of NaNs through the bright source is evident.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) and (b) Plot on the left shows a histogram of all stars after they have been passed through the Monte Carlo PSF correction method in the i + r coadded image. Sigma clipping is necessary to reject the stars on the right tail, which are not suitable for calculating the PSF. The graph has been truncated at x = 3 pixels. A similar graph for galaxies is shown on the right. This graph has been truncated at x = 10 pixels. (c) and (d) Plot on the left shows a histogram of all stars after they have been passed through the Monte Carlo PSF correction method in the i + r coadded images simulated using PhoSim with input γ 1 = 0.1. The plot is truncated at x = 3.5 pixels. Not all stars shown in the histogram are used for PSF correction. Sigma clipping is required to reject the stars on the right tail, which are not suitable for calculating the PSF. A similar graph for galaxies is shown on the right. This plot is truncated at x = 10 pixels.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: Median of background photon counts vs. variance of background photon counts for all chips in every image in the g, r, and i bands. Shown in red is the y = x + 300 while the black line is y = x. The yellow line shows the y = 0.9x line. If a chip is outside the strip which is defined by the red and yellow lines in over half the images, the chip is rejected. This condition was found to be effective in identifying severely defective chips.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: Normalized histogram of seeing (in arcseconds) for 151 r-band, 146 i-band, 161 g-band, and 141 z-band images. We excluded the u band since the image quality is extremely poor and only a few stars are detectable in the entire image. The seeing values are the FWHM size of the stars as calculated by QuickReduce.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: Red, green, and blue (RGB) color image of the full field containing the galaxy cluster A2390. We use the coadded images in the z, i, and r bands, which correspond to the R, G, and B channels, respectively. The field of view is approximately ﹩43^{\prime} ﹩ × ﹩49^{\prime} ﹩.