adsabs/AstroCLIMB huggingface dataset:
Paper: Gear Up for the Action Replay: Leveraging Lensing for Enhanced Gravitational-wave Early Warning
Authors: Sourabh Magare, Shasvath J. Kapadia, Anupreeta More, Mukesh Kumar Singh, Parameswaran Ajith, A. N. Ramprakash
Figure caption: Top left panel: simulated redshift distributions of BNSs detectable in various observing scenarios (O5, Voyager, 3G). The solid histograms correspond to distances LIGO–Virgo–KAGRA would infer assuming μ = 1 for lensed BNSs. The dotted histograms pertain to unlensed BNSs. We additionally show the expected intrinsic source redshift distribution (orange). Top right panel: same as the left panel but for NSBHs. Bottom left panel: magnification distribution for lensed BNSs pertaining to different observing scenarios (O5, Voyager, 3G). Bottom right panel: same as the left panel but for NSBHs.
Paper: Small Region, Big Impact: Highly Anisotropic Lyman-continuum Escape from a Compact Starburst Region with Extreme Physical Properties
Authors: Keunho J. Kim, Matthew B. Bayliss, Jane R. Rigby, Michael D. Gladders, John Chisholm, Keren Sharon, Håkon Dahle, T. Emil Rivera-Thorsen, Michael K. Florian, Gourav Khullar, Guillaume Mahler, Ramesh Mainali, Kate A. Napier, Alexander Navarre, M. Riley Owens, Joshua Roberson
Figure caption: The UV slope map of the entire galaxy (i.e., “arc 3” in Figure 1). The zoom-in view of the leaking region shows the distinctly blue UV slope of the leaking region compared to any other nonleaking regions of the galaxy. Consistent with previous figures, the β map suggests that the escape of LyC photons in the Sunburst Arc is primarily driven by a local, compact starburst region that is likely harboring a young star cluster(s) (Section 4.1).
Paper: The Cosmic Ultraviolet Baryon Survey: Empirical Characterization of Turbulence in the Cool Circumgalactic Medium
Authors: Hsiao-Wen Chen, Zhijie Qu, Michael Rauch, Mandy C. Chen, Fakhri S. Zahedy, Sean D. Johnson, Joop Schaye, Gwen C. Rudie, Erin Boettcher, Sebastiano Cantalupo, Claude-André Faucher-Giguère, Jenny E. Greene, Sebastian Lopez, Robert A. Simcoe
Figure caption: Summary of the physical properties of individual components collected from the COS-LRG (e.g., Zahedy et al. 2019, solid red circles) and CUBS (e.g., Zahedy et al. 2021; Cooper et al. 2021; Qu et al. 2022, solid orange triangles and solid blue squares) programs. Panel (a) displays the measured Doppler parameters (b ion) for low-ionization metal species along the y-axis and those of H I (b HI) along the x-axis. Error bars represent the 68% confidence interval. The low-ionization lines included in the analysis are primarily the Mg II doublet recorded in ground-based high-resolution optical echelle spectra, supplemented with far-ultraviolet lines, such as C II and O II, from HST COS observations. The dotted lines mark the two extreme scenarios of pure nonthermal broadening (top) and pure thermal broadening (bottom for carbon and magnesium). Panel (b) displays the derived constraints on the nonthermal motion b NT and thermal temperature T based on comparisons between the line widths of hydrogen and the ions presented in panel (a). Upper limits for T and b NT are shown as left-pointing and downward-pointing arrows, respectively. Panel (c) displays the line width inferred thermal temperature T vs. the gas density inferred from photoionization models (e.g., Zahedy et al. 2019, 2021; Cooper et al. 2021; Qu et al. 2022). Dotted lines mark the expectations from constant thermal pressure models of nT = 10, 100, 1000 K cm−3, suggesting a scatter of more than two decades in the internal gas pressure among individual clumps (see also Qu et al. 2022).
Paper: The Cosmic Ultraviolet Baryon Survey: Empirical Characterization of Turbulence in the Cool Circumgalactic Medium
Authors: Hsiao-Wen Chen, Zhijie Qu, Michael Rauch, Mandy C. Chen, Fakhri S. Zahedy, Sean D. Johnson, Joop Schaye, Gwen C. Rudie, Erin Boettcher, Sebastiano Cantalupo, Claude-André Faucher-Giguère, Jenny E. Greene, Sebastian Lopez, Robert A. Simcoe
Figure caption: Nonthermal line width b NT determined from the observed absorption profiles of individual clumps vs. the clump size l cl determined from best-fit photoionization models. Different symbols indicate the sources of measurements described in Figure 1 and in the main text. Following Figure 1, upper limits on b NT (downward arrows) are shown for components exhibiting line widths largely consistent with expectations from the mass-dependent thermal term. The expectation of ﹩{b}_{\mathrm{NT}}\propto {l}_{\mathrm{cl}}^{1/3}﹩ from the Kolmogorov theory for subsonic turbulence is shown as the dashed line. The correlation between b NT and l cl appears to flatten beyond l cl ≈ 1 kpc in star-forming halos. The best-fit lines for LRG and star-forming halos at l cl < 1 kpc are shown in solid red and blue lines, respectively. The extrapolation to larger spatial scales are shown in dotted line. Uncertainties associated with the best-fit models are displayed in the corresponding color-shaded area, while the estimated intrinsic scatter σ int is indicated by the bar in the lower-right corner. See the text in Section 4 for details.
Paper: The Cosmic Ultraviolet Baryon Survey: Empirical Characterization of Turbulence in the Cool Circumgalactic Medium
Authors: Hsiao-Wen Chen, Zhijie Qu, Michael Rauch, Mandy C. Chen, Fakhri S. Zahedy, Sean D. Johnson, Joop Schaye, Gwen C. Rudie, Erin Boettcher, Sebastiano Cantalupo, Claude-André Faucher-Giguère, Jenny E. Greene, Sebastian Lopez, Robert A. Simcoe
Figure caption: Distribution of the inferred gas density n H and clump size l cl for individual components included in this study. Different symbols indicate the sources of measurements described in Figure 1 and in the main text. Long-dashed lines mark the expected n H–l cl relation for a fixed N H, while the dotted line marks the relation for a constant clump mass of 105 M ⊙. The shaded area marks the parameter space where the size of the clumps exceeds the Jeans length (the dashed–dotted line) and the clumps are expected to be unstable against gravitational collapse. Note that while survey sensitivities may prevent detections of small, low-density clumps (but see the discussion in Section 5.1), the absence of large, high-density clumps is not a result of selection bias.
Paper: The Cosmic Ultraviolet Baryon Survey: Empirical Characterization of Turbulence in the Cool Circumgalactic Medium
Authors: Hsiao-Wen Chen, Zhijie Qu, Michael Rauch, Mandy C. Chen, Fakhri S. Zahedy, Sean D. Johnson, Joop Schaye, Gwen C. Rudie, Erin Boettcher, Sebastiano Cantalupo, Claude-André Faucher-Giguère, Jenny E. Greene, Sebastian Lopez, Robert A. Simcoe
Figure caption: Kinetic energy transfer rate per unit volume, ﹩\rho \,{\sigma }_{v}^{3}/{l}_{\mathrm{cl}}﹩ vs. clump size l cl. The turbulent velocity ﹩{\sigma }_{v}=\sqrt{3}\,{\sigma }_{v}^{\mathrm{los}}﹩ is computed using ﹩{b}_{\mathrm{NT}}=\sqrt{2}\,{\sigma }_{v}^{\mathrm{los}}﹩. Different symbols indicate the sources of measurements described in Figure 1 and in the main text. Following Figure 1, upper limits (downward arrows) arise as a result of nonconstraining b NT. The parameter space at l cl > 1 kpc is grayed out due to the uncertain nature of b NT. Over the range of spatial scales from l cl ≈ 1 pc to ≈1 kpc, the energy transfer rate per unit volume displays a mildly increasing trend toward smaller scales with a median value of ≈6  ×  10−29 erg cm−3 s−1 at l cl ≈ 100 pc and 1 order of magnitude scatter.
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Left: temporal evolution of the flux spectra (Stokes I) of SN 2023ixf presented in this paper. A comparison between the two sets of observations obtained at the first epoch, namely MJDs 60,084.20 (day +1.4) and 60,084.39 (day +1.6) illustrates the evolution of N III lines on a ∼1 hr timescale. Vertical black solid lines indicate prominent emission features. Dashed horizontal lines indicate the zero-point of each flux spectrum with the corresponding color. Each spectrum is offset by a constant with the exception of day +9.5. The flux spectra on days +1.4, +2.5, and +3.5 are scaled by a factor of four, four, and two, respectively. Days +4.6 and +9.5 are presented without any scaling to the flux. Right: a zoomed-in view of the Hα profile of SN 2023ixf. The flux density is normalized relative to the continuum.(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Same as Figure 1, but for day +4.6 (epoch 4).(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Same as Figure 1, but for day +9.5 (epoch 5).(The data used to create this figure are available.)
Paper: Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf
Authors: Sergiy S. Vasylyev, Yi Yang, 轶 杨, Alexei V. Filippenko, Kishore C. Patra, Thomas G. Brink, Lifan Wang, Ryan Chornock, Raffaella Margutti, Elinor L. Gates, Adam J. Burgasser, Preethi R. Karpoor, Natalie LeBaron, Emma Softich, Christopher A. Theissen, Eli Wiston, WeiKang Zheng
Figure caption: Same as Figure 1, but for day +14.5 (epoch 6).(The data used to create this figure are available.)
Paper: On the Subparsec-scale Core Composition of FR 0 Radio Galaxies
Authors: Margot Boughelilba, Anita Reimer
Figure caption: SEDs of the two gamma-ray sources, for a magnetic field strength of 25G in the jet. Top: SED of LEDA 55267. The dotted line is the modified blackbody modeling the host galaxy emission, the dashed line is the emission coming from the ADAF, the dashed–dotted line is the total jet’s emission, and the solid line represents the total emission of the source and is the sum of the three components. The differential fluxes sensitivities for 50 hr of observation with MAGIC (Aleksić et al. 2016) and H.E.S.S (Holler et al. 2015) are shown with the orange and purple dashed lines, respectively. Bottom: same for LEDA 58287.
Paper: On the Subparsec-scale Core Composition of FR 0 Radio Galaxies
Authors: Margot Boughelilba, Anita Reimer
Figure caption: SEDs of the 112 sources that are not individually detected in the gamma-ray band for a magnetic field strength of 25G in the jet. The faint blue lines are the individual fluxes of the 112 sources (see Section 4 for details), and the solid blue line is the average of the 112 models. The differential flux sensitivities for 50 hr of observation with MAGIC (Aleksić et al. 2016) and, H.E.S.S (Holler et al. 2015) are shown with the orange and purple dashed lines, respectively.
Paper: On the Subparsec-scale Core Composition of FR 0 Radio Galaxies
Authors: Margot Boughelilba, Anita Reimer
Figure caption: Same as Figure 2 but for B = 50G.
Paper: On the Subparsec-scale Core Composition of FR 0 Radio Galaxies
Authors: Margot Boughelilba, Anita Reimer
Figure caption: Same as Figure 3 but for B = 50G.
Paper: On the Subparsec-scale Core Composition of FR 0 Radio Galaxies
Authors: Margot Boughelilba, Anita Reimer
Figure caption: Broadband SED of FR Is (black dots), FR 0 s (green dots and green butterfly on right side), M87 in its 2017 quiet state (red stars). The blue star symbols are the SED of M87 with all the observations available in the NED. The butterfly plots in the very-high-energy gamma-ray range are the power-law spectra fitted to observations of the flaring state of M87 with H.E.S.S in 2005 (cyan region), VERITAS in 2007 and 2010 (purple and brown regions, respectively), and with MAGIC in 2008 (orange region). The SED of Tol 1326-379 is shown in yellow (data points on left side), including the butterfly plot at high-energy gamma rays (shaded area on right side), using the values derived by Grandi et al. (2016). The fluxes from FR Is have been rescaled from their mean distance to the mean distance of FR 0s (i.e., from a luminosity distance d L ∼ 1.5 × 1027 cm to d L ∼ 5.4 × 1026 cm). In the same way, M87 was rescaled to the mean distance of FR 0s. The data behind this Figure is available in the .tar.gz package. The package contains three .fits table files, a Python script, and a ReadMe. Included are 114 FR 0, 216 FR I, and one M87 SED table. The script can be used to read the data files. A list of all the sources is given in the Appendix Table 3.(The data used to create this figure are available.)
Paper: The Mass–Metallicity Relation of Dwarf Galaxies at Cosmic Noon from JWST Observations
Authors: Mingyu Li, 明宇 李, Zheng Cai, Fuyan Bian, Xiaojing Lin, Zihao Li, Yunjing Wu, Fengwu Sun, Shiwu Zhang, Emmet Golden-Marx, Zechang Sun, Siwei Zou, Xiaohui Fan, Eiichi Egami, Stephane Charlot, Gustavo Bruzual, Jacopo Chevallard
Figure caption: (a) The 1.″5 × 1.″5 red–green–blue or RGB (red for JWST/NIRISS F200W, green for F150W, and blue for F115W) cutouts, extracted 1D spectra, and corresponding 2D spectra for six galaxies in our sample. Their IDs, redshifts, and stellar masses are labeled. The flux density of 1D spectra, f  λ , is in unit of 10−19 erg s−1 cm−2 Å−1. (b) 1D spectral stacks binned by redshift and stellar mass, with each individual continuum-subtracted spectrum normalized by a dereddening flux of [O III] (see Section 3.3 for more details). The solid lines show the weighted average stacked spectra, and the shaded regions indicate the corresponding 1σ uncertainties. The low S/N wavelength ranges located at the edge of filter bands are masked. Emission lines are labeled as black dashed lines. The [O III]/[O II] line ratio evolves prominently with the stellar mass, demonstrating that galaxies with lower stellar mass tend to be more metal-poor.
Paper: The Mass–Metallicity Relation of Dwarf Galaxies at Cosmic Noon from JWST Observations
Authors: Mingyu Li, 明宇 李, Zheng Cai, Fuyan Bian, Xiaojing Lin, Zihao Li, Yunjing Wu, Fengwu Sun, Shiwu Zhang, Emmet Golden-Marx, Zechang Sun, Siwei Zou, Xiaohui Fan, Eiichi Egami, Stephane Charlot, Gustavo Bruzual, Jacopo Chevallard
Figure caption: The distribution of galaxies in our sample on the SFR-M ⋆ plane. The red squares show the z ≃ 2 sample, and the red hexagons show the z ≃ 3 sample. The MOSDEF stacked results are denoted in black triangles. The gray-shaded regions show the (extrapolated) galaxy main sequence at z = 2–3 based on the results from Speagle et al. (2014), Schreiber et al. (2015), Santini et al. (2017), Pearson et al. (2018), and Leja et al. (2022). The origin results from these works are denoted as gray dashed lines. The top and right panels show the stellar mass and SFR distributions respectively, with the z ≃ 2 sample in red, and z ≃ 3 sample in blue.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Probability density distributions of the offsets between the best-fitting line centroids of the O VII Kα, Kβ (RGS lines; black solid histogram) and O I, O II Kα (HRC-LETG lines; cyan solid histogram) absorbers from the samples of Nicastro et al. (2016b) and Nicastro et al. (2016a), respectively, and the rest-frame wavelengths of these transitions, together with their cumulative distributions (dashed black and cyan histograms, respectively). The inset shows the single O VII Kα, β (black points and 1σ statistical-only error bars) and O I, O II Kα (cyan points and 1σ statistical-only error bars) line centroid offsets as a function of the SNRE in the spectra.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Solid and dashed curves show, respectively, the 90% logN O VII  b contours as derived from the O VII Kα and Kβ transitions measured in the stacked X-ray–LLS (orange) and FUV–LLS (green) spectra of the X-ray halo. Light shaded orange and green regions show the 90% logN O VII  b solutions for the two spectra, further reduced into the dark shaded orange and green regions by the fiducial weighted-average value b O = 68 ± 10  km s−1 measured for O VI in the FUV spectra of our sample (black points with error bars). In this b O interval and in both the X-ray–LLS and FUV–LLS spectra, the 90% low-boundary constraint on the Kα (X-ray–LLS spectrum; lower solid orange line) or Kβ (FUV–LLS spectrum; lower dashed green line) transition sets solid and similar floors to the column density of O VII through the X-ray halo at a distance of 115 kpc from the galaxy center.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Constraints on the equivalent hydrogen column density of the X-ray halo at a projected distance 〈ρ〉 = 115 kpc, obtained by dividing the ion column densities of O VII (blue curves and shaded area), O VIII (brown curve and shaded area), and average O VI (green curve and shaded area; Fox et al. 2013) at the weighted-average 〈b O VI 〉 = 68 ± 10  km s−1 by their ion fractions in CIE gas (see Appendix D) and by the average Z = 0.3 Z ⊙ metallicity observed for our three cool CGM systems as a function of the temperature of the hot CGM gas. The H-like ion of oxygen is not detected in the X-ray halo spectrum, and its column density curve in the figure is a 90% confidence upper limit (brown curve and shaded region). Instead, O VI is detected in the FUV spectra but considered here as an upper limit to allow for at least a portion of this ion to be produced in physical phases different from the O VII-bearing phase. The left panel is for the stacked X-ray–LLS spectrum, while the right panel shows solutions for the FUV–LLS spectrum.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Two portions of the stacked X-ray–LLS (left panels) and FUV–LLS (right panels) frame spectra of the X-ray halo in continuum-normalized counts and wavelength ranges of 20.2–23 (top panels) and 17.3–20.1 (bottom panels) Å. The spectrum is binned at a resolution of 30 mÅ (about half the LSF FWHM of both instruments) and has SNRE = 29.3 in the continuum at λ = 21.6. The yellow curves are the best-fitting models. The fit yields combined (in quadrature) statistical significances of the O VII lines of 6.8σ (X-ray–LLS spectrum) and 4.7σ (FUV–LLS spectrum; Table 3).
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Fractional abundances of O VI (green), O VII (blue), and O VIII (brown) as a function of temperature (left panel) and hydrogen density (right panel) in CIE (left) and PIE gas illuminated by the average metagalactic radiation field at z = 0.276 (right).
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Same as Figure 9 but for the offsets (in  km s−1) between the O VII Kα, Kβ and O I, O II Kα line centroid differences measured in our RGS (black histograms) and HRC-LETG (cyan histograms) samples, respectively, and the corresponding expected line centroid differences.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: The O VII Kα (top panels) and Kβ (bottom panels) line EW-position confidence-level contours, up to the highest closed contour level, in the fits to the continuum-normalized stacked X-ray–LLS (left panels) and FUV–LLS (right panels) spectra of the X-ray halo. In each panel, the statistical significance of the highest closed contour is labeled for both one and two interesting parameters.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Constraints on the mass and temperature of the hot CGM in the X-ray halo as estimated from the X-ray–LLS (larger polygonal regions) and FUV–LLS (smaller polygonal regions) spectra for density spectral indices in the range β = 0.64–0.68 (isothermal halo) and hot CGM metallicity Z = 0.3 Z ⊙.
Paper: The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101
Authors: Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu
Figure caption: (a), (b) HST and (c), (d) Spitzer images of the site of SN 2023ixf. The SN position is shown by the cross-hair and the images have a dimension of 25″×25″. In the F658N narrowband image (a), a few H II regions are visible to the west and to the north of SN 2023ixf, and the gray-shaded stripe shows the slit position in one of our long-slit spectroscopic observations of the SN (Y. Zhang et al. 2023, in preparation); we extracted a spectrum from the red-outlined area in order to estimate the metallicity of the ionized gas (Section 4.1). In (a) and (b), the circle is centered at the SN position with a radius of 150 pc, within which we selected stars for an environmental analysis (Section 4.2). (e)–(h) Stamps of HST images in the F435W, F555W, F675W, and F814W bands, all with a dimension of 3″×3″. All panels are aligned north up and east to the left.