adsabs/AstroCLIMB huggingface dataset:
Paper: Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
Authors: R. Bandyopadhyay, C. M. Meyer, W. H. Matthaeus, D. J. McComas, S. R. Cranmer, J. S. Halekas, J. Huang, D. E. Larson, R. Livi, A. Rahmati, P. L. Whittlesey, M. L. Stevens, J. C. Kasper, S. D. Bale
Figure caption: Our fits are shown in solid black lines, and the previous fits from Cranmer et al. (2009) are plotted in dashed black lines.
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: Median (top) of the predicted time delays and the corresponding full width of the 68% confidence interval (bottom) shown for the double and quad configurations over a grid spanning the source plane. The coordinates y 1, y 2 are dimensionless source-plane coordinates and defined in Appendix B. The time delays of the images (labeled as A, B, C, and D and ordered by arrival time) are computed with respect to the time of arrival of the first image (A). The lens configuration parameters are q = 0.54, v = 111 km s−1, z  l  = 0.07, and z  s  = 0.22. These parameters correspond to a detectable lensed BNS for at least one point within the outer caustic. The detectability criterion is that any two images (out of A, B, C, and D) have S/N > 8. Out of the total quads (doubles), about 90% (21%) are detectable. While both the median and confidence interval increase as the source moves away from the center, the uncertainties are mostly less than a day, such that the relative error on the time delay spans 0.2–2.
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: time delay distributions (rendered as cumulative histograms) for detectable lensed BNS events in various observing scenarios. The fraction of events (y-axis) that cross a time delay threshold (x-axis) can be read off directly from the plot. The histogram of the total number of lensed BNS events is also plotted. As the sensitivity of the observing scenarios increases, the distributions converge toward the histogram of the expected number of lensed events. Correspondingly, the fraction of large time delays also increases. Top right panel: same distributions as the top left panel but shown separately for doubles (dotted) and quads (dashed). The detectable quads typically have smaller time delays than the doubles. Bottom left and right panels: same as the top left and right panels, except the sources are NSBHs. The detectable time delays are typically larger than the corresponding time delays for BNSs. This can be attributed to the larger horizon distance of GW detector networks for NSBHs compared to BNSs and a resulting increased fraction of larger time delays.
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: Full width of the 68% confidence interval, pertaining to image time delay predictions from host galaxy images. The time delays—computed with respect to the time of arrival of the first detectable image—and corresponding absolute widths of the confidence interval increase as both redshifts increase, although the relative error remains confined to 0.7–1.3.
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: Example illustrating the number of images produced based on the position of the source with respect to the caustics. When the source (green star) lies inside the inner caustic, four images (green circles) are produced. When the source (blue star) lies between the inner and outer caustics, two images (blue circles) are produced.
Paper: Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts
Authors: Immanuel Christopher Jebaraj, Vladimir Krasnoselskikh, Marc Pulupa, Jasmina Magdalenic, Stuart D. Bale
Figure caption: Statistics of spectral characteristics obtained from the analysis of 31 type III F–H pairs. Panel (a) shows a 15 minute interval on 2021 November 22 where 14 out of 17 type III bursts are F–H pairs. Panel (b) shows an example of a typical type III radio burst with F–H emission and fine structures observed on 2021 November 21. The dashed lines represent the frequency (1.5 MHz) and time (23:42 UT) slices from the spectrogram, which are presented in panels (c) and (d). In panels (a) and (b), the x-axis marks the observer’s distance from the Sun. The data points (blue triangles for F and yellow circles for H) are fitted with an exponentially modified Gaussian (red curve). Here τ  r  and τ  f  are the rising and falling times, and τ peak is the peak intensity. The statistics of the f H/f F ratio and the f F − f H propagation delay as dependencies of frequency are presented in panels (e) and (f). Panels (g) and (h) present the intensity and bandwidth as a function of the frequency, respectively. The F and H are represented by the blue triangles and yellow circles. For a one-to-one comparison with F, the results of H are presented as f H/2. The average background noise (QTN + galactic) is illustrated in panel (f) by the red line, which scales as 1/f 2.2±0.4. The vertical red line and red shaded region in panel (g) mark the peak bandwidth and its spread.
Paper: Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts
Authors: Immanuel Christopher Jebaraj, Vladimir Krasnoselskikh, Marc Pulupa, Jasmina Magdalenic, Stuart D. Bale
Figure caption: Time profile characteristics of the 31 type III F–H pairs. Shown is the rising time of F (blue triangles) and H (yellow circles) as a function of frequency in panel (a) and intensity in panel (b). The one-to-one relationship between the rising times of F and H is shown in panel (c). The falling time of F and H as a function of frequency is presented in panel (d), while the time profile asymmetry (τ  f /τ  r ) as a function of intensity is shown in panel (e). The time delay between the F and H components at the rising and falling phases (at half-power) and peak power as a function of frequency is shown in panel (f).
Paper: Fundamental–Harmonic Pairs of Interplanetary Type III Radio Bursts
Authors: Immanuel Christopher Jebaraj, Vladimir Krasnoselskikh, Marc Pulupa, Jasmina Magdalenic, Stuart D. Bale
Figure caption: Examples with polarization. The top panels show the Stokes intensity I parameter from HFR and LFR for the same example type III burst shown in Figure 1(a) and a longer 15 minute time period on 2021 November 22 (panel (b)). The middle panels show the corresponding relative Stokes polarization V/I. Separate polarized components are visible for both F and H components of the burst. The bottom panels show the magnetic field in RTN coordinates, with the field dominated by a negative (sunward) radial component.
Paper: Coronal Heating Rate in the Slow Solar Wind
Authors: Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Cooper Downs, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Lingling Zhao, Alessandro Liberatore, Chen Shi, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Arkadiusz Berlicki, Roberto Bruno, Gerardo Capobianco, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D'Amicis, Michele Fabi, Fabio Frassetto, Marina Giarrusso, Silvio Giordano, Salvo L. Guglielmino, Enrico Magli, Giuseppe Massone, Mauro Messerotti, Giuseppe Nisticò, Maria G. Pelizzo, Fabio Reale, Paolo Romano, Udo Schühle, Sami K. Solanki, Thomas Straus, Rita Ventura, Cosimo A. Volpicelli, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella, Stuart D. Bale, Justin C. Kasper
Figure caption: Data-based (black) and physics-based (red) modeling of the radial evolution of the solar wind U (thick lines) and Alfvén U  A  (thin lines) speed (a), plasma mass density ρ (b), solar wind flux energy F  w  (c), magnetic field B (d), turbulent energy E  b  (e) and correlation length λ  b  (f), and heating rate ϵ (g) in the slow coronal flow, jointly observed with SO/Metis and PSP during their quadrature on 2022 June 1. The blue dot in each panel refers to the values obtained with PSP measurements. The Parker classical model for an expanding isothermal 1.5 MK corona is shown as a green line in (a).
Paper: Coronal Heating Rate in the Slow Solar Wind
Authors: Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Cooper Downs, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Lingling Zhao, Alessandro Liberatore, Chen Shi, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Arkadiusz Berlicki, Roberto Bruno, Gerardo Capobianco, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D'Amicis, Michele Fabi, Fabio Frassetto, Marina Giarrusso, Silvio Giordano, Salvo L. Guglielmino, Enrico Magli, Giuseppe Massone, Mauro Messerotti, Giuseppe Nisticò, Maria G. Pelizzo, Fabio Reale, Paolo Romano, Udo Schühle, Sami K. Solanki, Thomas Straus, Rita Ventura, Cosimo A. Volpicelli, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella, Stuart D. Bale, Justin C. Kasper
Figure caption: (a) Metis pB image on 2022 June 1 at 22:40 UT with PSP marked in its POS as a blue dot; the PSP direction is indicated by a white dashed line. (b) Projection of the PSP position (blue dot) onto the Carrington map of the squashing factor Q at 10 R ⊙. (c) PSP magnetic field and plasma time series (from top to bottom: wind bulk and Alfvén speed, magnetic field intensity and angle with the radial, and proton density and temperature) during the quadrature with SO. (d) Radial profile of the Metis pB observations at the latitude corresponding to the PSP location (open squares), along with the van de Hulst (1950) power-law fit (red line); the horizontal line at 1.2 × 10−11 B/B ⊙ represents the flattening level, probably due to the contamination by the F-corona and instrumental effects.
Paper: High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and Their Impact on the Leavitt Law and the Hubble Constant
Authors: Anupam Bhardwaj, Adam G. Riess, Giovanni Catanzaro, Erasmo Trentin, Vincenzo Ripepi, Marina Rejkuba, Marcella Marconi, Chow-Choong Ngeow, Lucas M. Macri, Martino Romaniello, Roberto Molinaro, Harinder P. Singh, Shashi M. Kanbur
Figure caption: High-resolution ESPaDOnS spectra for all 42 MW Cepheid standards in the range 6000–6050 Å. The star IDs are provided on the right and the vertical dashed lines mark the positions of atomic lines.
Paper: Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 < z < 9: Evidence for Very Early Formation of the Central ∼100 pc of Present-day Ellipticals
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Ivo Labbé, Gabriel Brammer, Tim B. Miller, Rachel Bezanson, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Katherine A. Suess, Erica J. Nelson
Figure caption: Left: the stellar mass profiles for the nine well-fit galaxies in F200W derived from r  e  and n in Table 1. The median profile is shown in black, along with the (16%, 84%) quantile range (see text). Right: the median stellar mass profiles compared to stellar mass profiles of compact massive quiescent galaxies at z ∼ 2.3 and massive elliptical galaxies at z = 0 obtained from Bezanson et al. (2009). The central densities are remarkably similar, consistent with inside-out growth over the entire redshift range.
Paper: Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 < z < 9: Evidence for Very Early Formation of the Central ∼100 pc of Present-day Ellipticals
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Ivo Labbé, Gabriel Brammer, Tim B. Miller, Rachel Bezanson, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Katherine A. Suess, Erica J. Nelson
Figure caption: Effective radius along major axis vs. stellar mass for the nine galaxies in F200W. The stellar masses and their errors are taken from L23. We show the tracks for the full population of galaxies for z ∼ 0.35 (light gray), z ∼ 2.75 (gray) obtained from Mowla et al. (2019), a size–mass relation at z ∼ 5 derived from Shibuya et al. (2015; solid dark gray; see text) and two massive galaxies at z > 7 reported by Akins et al. (2023; red triangle; see text). The size–mass relation of simulated galaxies at z = 7 in the BLUETIDES cosmological hydrodynamical simulation is shown by the black dashed line (Marshall et al. 2022; see Section 5).
Paper: Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 < z < 9: Evidence for Very Early Formation of the Central ∼100 pc of Present-day Ellipticals
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Ivo Labbé, Gabriel Brammer, Tim B. Miller, Rachel Bezanson, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Katherine A. Suess, Erica J. Nelson
Figure caption: The top row shows 1″ × 1″ images in the NIRCam F200W band of the nine galaxies for which a good Sérsic fit was found. The second row shows the masks that were used, the third the best-fitting GALFIT models. The residuals, obtained by subtracting the best-fitting models from the images, are shown in the fourth row. The bottom row shows RGB images of the galaxies, with F150W as the blue band, F277W as the green band, and F444W as the red band.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec AGN (VODKA). SDSS J1608+2716: A Subarcsecond Quadruply Lensed Quasar at z = 2.575
Authors: Junyao Li, Xin Liu, Yue Shen, Masamune Oguri, Arran C. Gross, Nadia L. Zakamska, Yu-Ching Chen, Hsiang-Chih Hwang
Figure caption: Comparison of the stellar mass of the foreground lens estimated from lens modeling (black curve) and stellar population analysis (shaded regions) as a function of the assumed redshift of the lens. The age of the main stellar population is fixed to either the age (blue) or half the age (pink) of the Universe at a given redshift. The lower and upper edges of the shaded region correspond to E(B − V)line = 0.0 and E(B − V)line = 1.0 assumed in the stellar model, respectively.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec AGN (VODKA). SDSS J1608+2716: A Subarcsecond Quadruply Lensed Quasar at z = 2.575
Authors: Junyao Li, Xin Liu, Yue Shen, Masamune Oguri, Arran C. Gross, Nadia L. Zakamska, Yu-Ching Chen, Hsiang-Chih Hwang
Figure caption: Comparison of the (a) observed image with the (b) reconstructed image from lens modeling. Also shown are the (c) normalized fitting residual, the (d) reconstructed quasar position (marked by the star) and its host galaxy, a plot of the (e) unitless convergence and (f) magnification, as well as the (g) extended surface brightness of the foreground lens, the (h) lensed quasar host galaxy, and the (k) lensed quasar + quasar host. Model images shown in panels (b) and (k) have been convolved with the PSF.
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: Lyα escape fraction (f esc(Lyα)) vs. β (left) and [O III]/[O II] vs. f esc(Lyα) (right) relations for the leaking region, the nonleaking regions, and the entire galaxy. The format is the same as in Figure 2. Combined with the very blue β and high [O III]/[O II] ratio, the leaking region is clearly characterized by relatively high f esc(Lyα), the presence of extreme stellar populations, and a highly ionized nebular state (Sections 4.1 and 4.2). It also implies a physical connection between LyC and Lyα escape processes on subkiloparsec scales such that the LyC-leaking region features a higher escape fraction of Lyα as well, likely due to the preferred low N(H I) channels for both photons (Section 4.3).
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: Left: [O III]/[O II] vs. UV-continuum slope (β) for the leaking region (black), the nonleaking regions (red), and the entire galaxy (blue) as marked in Figure 1. The light gray and pink circles with error bars indicate the mean value and 1σ population deviation of each region. Right: same as the left panel but for [O III]/Hβ. In the Sunburst Arc, the multiple lensed images of the LyC-leaking region (black) show the remarkably blue UV-continuum slope β ≃ −2.9 and the high ionization state of the surrounding ISM ([O III]/[O II] = 11 ± 3 and [O III]/Hβ = 6.8 ± 0.4), which is distinctly extreme compared to the nonleaking regions (red) and the entire galaxy (blue). The leaking region’s extremely blue β and high ionization–sensitive line ratios (corresponding to an ionization parameter ﹩\mathrm{log}U﹩ of ≃−2; Section 4.1) suggest that LyC photons are produced and escape from a local, highly ionized compact region with extreme stellar populations (Section 4).
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 HST color-composite images of the strongly lensed LyC galaxy (Sunburst Arc at z = 2.37), showing its spatially resolved morphology. The image filters (red: F140W; green: F606W; blue: F410M) trace the rest-frame optical, UV-continuum, and Lyα emission, respectively. The galaxy appears as four arcs due to the strong lensing effect of the foreground galaxy cluster PSZ1 G311.65–18.48 at z = 0.44 (Dahle et al. 2016; Sharon et al. 2022). Across the arcs, a LyC-leaking starburst region appears multiple times, as marked with yellow circles (i.e., 1–12). The lensed images of the leaking region have different lensing magnifications as computed from the lens model (Sharon et al. 2022). Each image also has a slightly different viewing angle from us. The nonleaking regions used in our analysis are marked as red circles in the arc 1 and 2 images. We also measure the galaxy-integrated physical properties from the entire galaxy region outlined in green in the arc 3 image.
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: Illustrative diagram of the anisotropic viewing geometry for LyC escape in the Sunburst Arc. Case A is the pencil-beam viewing geometry suggested for the galaxy, where LyC photons directly escape from the ionizing star cluster through a highly ionized, low N(H I) hole(s) that opens toward our line of sight. In this viewing geometry, we may be staring “down the barrel” of the inner hot H II region of the ionizing star cluster, enabling us to observe LyC photons and pristine stellar light that are minimally attenuated by neutral hydrogen and dust, as indicated by the very blue β ≃ −2.9 of the leaking region (Section 4.4). This anisotropic LyC escape process through specific opening angles implies that if we view the galaxy from most other angles, we may not see escaping ionizing photons and thus might identify it as a nonleaker, which is depicted as case B. Thanks to strong lensing magnification, our analysis isolates the physical properties of the leaking region (blue stars) from the nonleaking regions (orange stars). The size (r star ≲ 32 pc) of the ionizing star cluster is an upper limit due to the HST’s spatial resolution and is estimated from the strong lens model analysis of Sharon et al. (2022).
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 comparison of the leaking region’s UV slope with starburst population models suggests that the leaking region’s UV light is dominated by “pure” stellar light (i.e., minimal contribution from nebular continuum emission and extinction by dust). The age (∼3 Myr) of the leaking region is adopted from the far-UV SED modeling in Chisholm et al. (2019). Both the “stellar+nebular” and “pure stellar” models assume the same constant star formation history and subsolar metallicity of 0.4 Z ⊙, which is similar to the metallicity derived from Chisholm et al. (2019). The starburst population models are adopted from Schaerer (2003). The leaking region’s β, consistent with the “pure stellar” model, suggests that the leaking region’s UV emission nearly exclusively consists of uninterrupted direct starlight, with minimal contributions from nebular continuum emission and negligible dust extinction. Such direct starlight from the leaking region indicates the presence of small ionized channels through which LyC photons escape (Section 4.2).
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 HST filters and photometric SED fits to subtract off the underlying continuum flux from the narrowband emission lines (Section 2.5). On-band filters are shown with solid curves; off-band continuum filters are plotted as dotted–dashed curves. The y-axis is the filter throughput. The best-fit spectra used to determine the continuum fits are overplotted as solid lines, with arbitrary scaling (different in each plot, so as not to obscure the filter curves) in f  λ  (units of erg s−1 cm−2 Å−1). Each of the solid lines corresponds to each of the multiple images of the whole galaxy contained in arcs 1 and 2. In the top panel, the emission line Lyα is overplotted with arbitrary flux. In the bottom panel, the following emission lines are overplotted with arbitrary flux: the [O II] doublet, which falls in the F126N filter; Hβ, which falls in the F164N filter, [O III] λ4959, which falls in the F1647 filter; and [O III] λ5007, which falls just outside the F167N filter.