adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Left: Flamingos-2 stacked J-band image of WISEA 1534−1043. North is up and East is to the left. The image is approximately 20″ on a side. The blue circle centered on the location of WISEA 1534−1043 is 1.″4 in diameter. Two relatively bright and nearby galaxies are labeled as “1” and “2” in red text. Right: same as left, but with galaxies “1” and “2” each modeled as a two-dimensional Gaussian light distribution and subtracted, to better reveal the WISEA 1534−1043 counterpart.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Color–color diagram (adapted from Meisner et al. 2021) highlighting candidate extreme T-type subdwarfs and updated to reflect the J-band results of our Gemini follow-up imaging campaign (black dots). The other samples shown are L dwarfs (blue), young L dwarfs (cyan), L subdwarfs (green), “normal” T dwarfs (magenta), young T dwarfs (brown), T subdwarfs (orange), esdT candidates from Schneider et al. (2020; red; W0414 = WISEA 0414–5854, W1810 = WISEA 1810–1010), and members of our present Gemini sample with J magnitudes from the prior literature (yellow stars). Note the location of WISEA 1534−1043 near the very upper middle. The shaded gray box indicates the fiducial esdT candidate color–color selection proposed in Meisner et al. (2021). Dotted black lines show our model tracks for [m/H] = 0 and [m/H] = −0.5 (labeled in black text near the upper right end of each track). Both of these model tracks have log(g) = 5, log(K  zz ) = 7, and γ = 1.25 (Tremblin et al. 2015). CWISE 0738−6643 (labeled W0738) stands out as unusually red in J − W2 for its modest W1 − W2 color, even among the sample of esdT candidates. CWISEP J050521.29−591311.7 (labeled W0505), CWISEP 0905+7400 (labeled W0905; Meisner et al. 2020a), and WISE J201404.13+042408.5 (labeled W2014; Kirkpatrick et al. 2012) are also individually labeled because they fall just outside of the fiducial esdT color–color selection box. The early T subdwarf candidate labeled W1230 is CWISE J123041.80+380140.9 from Kota et al. (2022).
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: The F110W − J color of WISEA 1534−1043 (red shaded region) compared to F110W − J color synthesized from Hubble Space Telescope spectroscopy of 14 late T and Y dwarfs (blue data points; Cushing et al. 2011, 2014, 2021; Kirkpatrick et al. 2012; Schneider et al. 2015). There is a roughly linear trend between F110W − J color and numerical spectral type (T0 = 0, Y0 = 10). The blue dashed line shows a linear fit to the comparison sample (excluding W1534) and the gray envelope shows the 1σ linear fit confidence interval. The Pearson correlation coefficient of the comparison sample in terms of F110W − J vs. spectral type is −0.89, indicating a strong negative correlation. W1534 has a bluer F110W − J color than the other late T and Y dwarfs, such that the 1σ upper envelope of its F110W − J color remains bluer than the bluest F110W − J color in the comparison sample. This indicates that WISEA 1534−1043 has an unusual spectrum in the 0.9–1.4 μm range relative to the known population of brown dwarfs currently thought to be similar in temperature.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Reduced proper motion diagram for members of our sample with Gemini J-band detections (black points), L subdwarfs (green), T subdwarfs (orange), esdT candidates from Schneider et al. (2020; red; W0414 = WISEA 0414–5854, W1810 = WISEA 1810–1010), and known Y dwarfs (gray). Ross 19B and CWISEP 0156+3255 (labeled W0156) are indicated with yellow stars because they are members of our Gemini sample with J-band detections from the prior literature (Meisner et al. 2020a; Schneider et al. 2021). Some of the Y dwarfs which appear most extreme in this diagram are individually labeled: W0402 = CWISEP J040235.55−265145.4 (Meisner et al. 2020a), WD0806B = WD 0806−661B (Luhman et al. 2011), W0830 = WISEA 0830+2837 (Bardalez Gagliuffi et al. 2020), W0855 = WISE 0855−0714 (Luhman 2014b), and W1828 = WISEPA J182831.08+265037.8 (Cushing et al. 2011; Kirkpatrick et al. 2011).
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Our new Gemini Y-band detection of Ross 19B allows us to further place it in context with the population of late T and early Y dwarfs. Left: Y MKO − J MKO color as a function of spectral type, for the population of known late T and Y dwarfs (black squares with vertical error bars). The Y MKO − J MKO measurement for Ross 19B is shown as a shaded red rectangle. Right: Y-band absolute magnitude vs. spectral type for late T and Y dwarfs, plus our Ross 19B measurement in red. In both panels the dashed black line shows the mean trend for known objects as a function of spectral type. The Y MKO − J MKO color and M  Y  measurements for Ross 19B favor a spectral type between T9 and Y0.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: A metallicity sequence of models from Tremblin et al. (2015). All models have T eff = 500 K, log(g) = 5, and log(K  zz ) = 6. Red, green, and blue lines are the [m/H] = 0, −0.5, and −1 dex models, respectively. All models are normalized to unity between 0.91 and 0.925 μm. The dotted–dashed black line shows the Gemini/Flamingos-2 Y-band transmission, the thin solid black line shows the F110W transmission, and the dashed black line provides the MKO J-band transmission. These transmission curves are displayed here with normalizations such that each has a maximum value of 4. As metallicity decreases, the J-band peak is dramatically suppressed such that a bluer color arises within the 0.9–1.4 μm wavelength range. Thus, the Tremblin et al. (2015) models appear qualitatively in alignment with the relatively blue F110W − J color of WISEA 1534−1043.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Comparison of WISE W1/W2 and Spitzer ch1/ch2 photometry for mid–late T dwarfs, Y dwarfs, and T/Y subdwarf candidates. W2 and ch2 remain tightly correlated with effectively zero systematic offset across the range of M W2 and J − W2 values spanned by this sample. On the other hand, there is considerable scatter between W1 and ch1 magnitudes, with this scatter becoming larger for increasing M W2, W1, and J − W2. This suggests that caution ought to be exercised when attempting to select cold, low-metallicity candidates based on WISE W1 − W2 color only, as has been previously attempted/suggested in Meisner et al. (2021) and Brooks et al. (2022).
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Comparison of CatWISE2020 magnitudes fitted with (without) accounting for proper motion, w?mpro_pm (w?mpro), based on the sample of T and Y dwarfs shown in Figure 2. As the total proper motion (horizontal axis value) gets larger, a greater fraction of flux is “missed” by w?mpro, resulting in w?mpro magnitudes that are systematically too faint. We therefore caution that it is important to use w1mpro_pm and w2mpro_pm rather than w1mpro and w2mpro for objects with total motions ≳1″ yr−1, even though w1mpro_pm and w2mpro_pm are not the default CatWISE2020 fluxes provided via IRSA.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: The RVs of the targets and fittings. The filled circles and triangles represent RV observations of primary and secondary components, respectively. Small gray symbols denote data from different sources besides APOGEE-2: APOGEE-1 for RV CVn, TNO for EK Com, and LAMOST for V384 Ser and EH CVn. The dotted lines give the respective point circular orbit (sine-curve) fits, while the solid lines give the RV curves, which are calculated from the best solutions (taking into account the proximity correction) of each object. The dashed lines in a few panels denote solutions from optional results (explained in the text) for comparison. The horizontal bars stand for half the exposure time.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: The q–﹩\overline{{\rm{\Sigma }}}﹩ curves (left panels) and phased light curves (right panels) for RV CVn, EK Com, and V384 Ser. The target names are listed in the left panels. In the right panels, the symbols and thick blue solid lines denote the observed and synthetic (best solutions) light curves, while the thin gray dotted lines represent the theoretical light curves without a smear effect. In the middle right panel, the calculated curve from optional results is shown by the orange dashed line. The residuals of the light curves are shown at the bottom of each panel. The label “s” denotes the TESS sector.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: The CCF profiles of the targets and multi-Gaussian fittings for RV CVn, EK Com, and V384 Ser. The multi-Gaussian components are shown with thin blue dotted lines, while the linear or quadratic components are shown with thick blue dotted lines, and the final fitted profiles are shown with yellow dashed lines. The phases are shown in the upper right of each panel.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Analysis of the TESS SLCs of V384 Ser. Top left: variation of the light curves indicated from ﹩-{\rm{\Delta }}\mathrm{Max}﹩ and ﹩-{\rm{\Delta }}\mathrm{Min}﹩. Bottom left: comparison of light curves of different segments. Top right: observed and calculated light curves. Bottom right: SLCs and fittings from the results of LLCs. The blue solid lines represent theoretical light curves, while the orange dashed lines denote calculated light curves without a smear effect. Except for the top left panel, all light curves shown are rebinned from the  original data. The light curves are vertically shifted for clarity.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Same as Figure 2 but for V1038 Her, EH CVn, and J125403.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Aperture photometry of the targets. The top and middle panels show the observed images and the corresponding apertures (yellow for the aperture and blue for the background), respectively. The extracted light curve of RV CVn is shown in the bottom panel.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Spectra of V384 Ser and EK Com (a zoomed-in view) from APOGEE. The lower spectrum is vertically shifted. The MJDs of the spectra are listed on the left.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Normalized spectra of RV CVn from APOGEE-1. The spectra are vertically shifted for clarity. The MJD of each spectrum is marked on the left side.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Multiband light curves of V1038 Her and the theoretical fittings.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Same as Figure A1 but for EK Com from the observations at TNO.
Paper: Comparative Study of TESS Photometry and Radial Velocities on Six Early K-type Contact Binaries with Similar Periods around 0.268 Day
Authors: N.-P. Liu, S.-B. Qian, W.-P. Liao, Y. Huang, Z.-L. Yuan
Figure caption: Same as Figure A1 but for V1038 Her, EH CVn, and J125403.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: (Left) The population of stellar companions ranging from 7–150 M J in eccentricity and semimajor axis, colored by the apparent magnitude. (Right) The same population in radius and mass, colored by the effective temperature of the host star. Vertical lines at 13 M J and 80 M J denote the traditional boundaries of the BD regime. The solid black line shows the ATMO 2020 substellar evolutionary model (Phillips et al. 2020) for HIP 33609 b’s measured age (150 ± 25 Myr) with the green shaded regions depicting the 1, 2, and 3σ uncertainties. Note: systems where the primary body is a BD or white dwarf are not included. References: Bakos (2010), Buchhave et al. (2011), Tingley et al. (2011), Parviainen et al. (2014), Bonomo et al. (2015), Esteves et al. (2015), Stassun et al. (2017), Bento et al. (2018), Cooke et al. (2020), Cortés-Zuleta et al. (2020), Grieves et al. (2021), Carmichael et al. (2022), Gill et al. (2022), Psaridi et al. (2022), Sebastian et al. (2022).
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB estimation algorithms are able to mask areas of an image containing light from discrete objects or bright sky gradients. The top row shows two example images in our SKYSURF database. The bottom row shows corresponding ProFound SKY maps, with the borders of Pro-med subregions overlaid. The bottom left ProFound map corresponds to the top left image, and similarly for the rightmost images. The subregions used for the Pro-med algorithm are overlaid with white or red borders. Red subregions are identified by our algorithms as likely containing light contamination, and are masked during sky-SB estimation. We show these images to demonstrate our ability to reject areas of an image, but emphasize that images like this are rejected for sky-SB analysis because they are too crowded, as identified by the amount of red subregions.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB measurements vs. ecliptic latitude for WFC3/UVIS (UV filters), zoomed in to show the range between −0.1 and 0.3 MJy sr−1.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Flowchart of the ProFound Median (Pro-med) pipeline to estimate the sky-SB from an HST image.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB measurements vs. ecliptic latitude for WFC3/UVIS (Optical filters), zoomed in to show the range between 0 and 0.5 MJy sr−1. There is a larger scatter in the F850LP filter due to the high sky-SB rms of this filter.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: An extinction-corrected CMD for NGC 7789 using GAIA photometric data. As identified in the plot legend, the star-shaped symbols show the red giants of this study. The reddening vector shows the direction and length by which we shifted the stars on the CMD to correct for interstellar reddening effects.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Spectra of the Li I λ6707 resonance transition in all NGC 7789 red giants observed with the Tull Spectrograph (left panel) and of the He I λ10830 transition in all of this cluster’s stars observed with HET/HPF by Sneden et al. (2022; right panel). Attention is called to Li-rich stars 193 (in blue) and 301 (in red). All spectra of NGC 7789 giants observed with either instrument are shown in this figure.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Another CMD for NGC 7789 with the data from Figure 1, using colors to indicate the Li abundances for NGC 7789 members.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Observed and synthetic spectra for the two NGC 7789 stars with very high Li abundances. The λ6707 resonance lines shown in panels (a) and (c) are so saturated that they cannot yield reliable abundances. The weaker, higher-excitation λ6103 lines in panels (b) and (d) are better Li features for these two stars. (Sneden et al. 2022). In the legend of each panel, “best” indicates the synthesis using the abundance derived for the named element, and “no” indicates the synthesis computed without any contribution of this element. The other syntheses have abundance offsets (in dex) as indicated in the legends.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Carbon isotopic ratios (panel (a)) and CNO abundances (panels (b)–(d)) as functions of Li abundance in all NGC 7789 program stars, including star 193, which is a probable nonmember of the cluster. The dotted lines in panels ((b)–(d)) indicate the solar abundance values. Star 193 is the blue dot and Star 301 is the red dot.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Correlation between lithium abundances and He absorption line strengths in Paper I and the present work. Identification of the points are in the figure legend.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Observed and synthetic spectra for the features used to determine C, N, and O abundances in star 501, a typical program star. The observed points are shown with open circles. The meanings of the legends in each panel are the same as in Figure 4.
Paper: Chemical Compositions Of Red Giant Stars in the Old Open Cluster NGC 7789
Authors: Neel Nagarajan, Christopher Sneden, Melike Afşar, Catherine A. Pilachowski
Figure caption: Comparison of NGC 7789 abundances in this paper to results from some previous papers. The various studies are identified by color types, as defined in the plot legend and are as follows: Overbeek et al. (2015), Jacobson et al. (2011), Pancino et al. (2010), and Tautvaišienė et al. (2005)
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Two-dimensional histograms of the darkest subregions for all the images in every filter in WFC3/IR. The color bar indicates the percentage of images (N Darkest/N Total × 100%, where N Darkest is the number of darkest subregions and N Total is the total number of images) in this filter that contain a darkest subregion in the corresponding location. In other words, regions that are more blue/purple have systematically lower sky-SB levels across the entire filter. White indicates regions that are always ignored due to detector artifacts. Known artifacts that are always masked are the “death star” (bottom middle) and “wagon wheel” (bottom right corner).