adsabs/AstroCLIMB huggingface dataset:
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Variations of ν and χ with time for ﹩{B}_{\max }^{\mathrm{tor}}\sim 9\times {10}^{16}﹩ G (and ﹩{B}_{\max }^{\mathrm{pol}}\sim 5\times {10}^{14}﹩ G), initial ν = 200 Hz, and χ = 3° (upper panel) and χ = 30° (lower panel). Red solid and blue dashed lines show the variations of ν and χ, respectively.
Paper: On the Blackbody Spectrum of Kilonovae
Authors: Albert Sneppen
Figure caption: The wavelength dependence of the spectral correction, f(β, λ)/f(β), for different velocities, v  bb  (left panel), cooling rates, α (center panel), and recession rates, a (right panel). These corrections are computed by convolving blackbodies over the photospheric surface and comparing to the best-fit single-temperature blackbody. Convolving over a range of effective temperatures results in a wider blackbody with a correspondingly less prominent peak. The wavelength on the lower x-axis is shown relative to the peak wavelength, λ peak, of the input blackbody, B  λ (T emitted(μ = 1)), while the top x-axis shows the corresponding wavelength assuming an emitted temperature of T emitted(μ = 1) = 4000 K. Left: spectral correction for different blackbody velocities, while holding the velocity (a = 0) and temperature constant (α = 0). Center: spectral correction given variable cooling rates and disregarding the relativistic Doppler corrections. To compute the characteristic time delays we use the characteristic velocity of AT2017gfo in Epoch 1, v  bb  = 0.28c. Right: amplification of the spectral correction introduced by different velocity recession rates, a, with a velocity at the nearest front of v  bb (μ = 1) = 0.28c and a constant temperature (α = 0).
Paper: On the Blackbody Spectrum of Kilonovae
Authors: Albert Sneppen
Figure caption: Spectra of AT2017gfo 1.43 days after the merger. Spectra are from the VLT/X-shooter spectrograph (gray), with best-fit blackbody and Sr+ P Cygni. Shaded bars indicate tellurics and ill-constrained or noisy regions at the edge of the UVB, VIS, and NIR arms of the spectrograph. Wavelength from 330 to 400 nm are not included as spectral modeling is sensitive to the ill-constrained line blanketing from Y+, Zr+, and other r-process elements (Gillanders et al. 2022; Vieira et al. 2023).
Paper: On the Blackbody Spectrum of Kilonovae
Authors: Albert Sneppen
Figure caption: Temperature at the photospheric surface as a function of angle, θ, between the line of sight and the direction of expansion for any surface element. Blue indicates the relativistic Doppler correction with β = 0.28. Red illustrates the impact of time delay, showing the temperature in the emitted frame relative to the front. This is computed assuming the temporal timescale of epoch 1 (1.43 days) and the cooling rate derived from fitting across epochs 1–5 from the X-shooter spectra (Sneppen et al. 2023a). The purple dotted line indicates the combined effect, which is relatively invariant across the surface elements.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: Shock diagnostics in the kinematic component of the J1652 quasar host galaxy. The top panels show log([S  II]/Hα) and log([O I]/Hα) emission-line-ratio maps where the bar represents 8.5 kpc and the red star shows the location of the quasar. Teal contours show the shock-ionization regions orthogonal to the outflow shown in white contours. We show the emission-line ratios of log([S II]/Hα) and log([O I]/Hα) as a function of the emission-line dispersion in the bottom panel with the black points. Median emission-line-ratio and velocity dispersion errors are shown with the red point in the lower right corner. We observe, on average enhanced line ratios with higher velocity dispersions in regions perpendicular to the quasar outflow and the ionization cone shown in the green points. Binned line ratios are shown with the blue curves. The orange curves represent a second-degree polynomial fit to all data points. The green curve shows a radiative shock model from Allen et al. (2008) for an electron density of 100 cm−3, solar metallicity, and magnetic field strength of 10 μG cm3/2.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: On the left, we present an extinction-corrected, Hα-derived star formation rate map in the quasar host galaxy of J1652, only selecting spaxels with emission-line ratios consistent with star formation ionization. In the center, we show a metallicity map. On the right, we show an electron density map. In each plot, we show a total Hα map in gray. We observe the brightest star-forming region to have lower metallicity and elevated electron density.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: Maps of emission-line ratios. We present emission-line-ratio maps for log([O  III]/Hβ), log([N  II]/Hα), log([S II]/Hα), and log([O  I]/Hα) for each distinct kinematic component in the bottom three rows. The top row shows the emission-line ratios integrated over the three kinematic components. The ellipse in the lower left corner shows the size of the NIRSpec-IFU PSF. North is up, and east is to the left.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: Schematic of the major components of J1652 as seen in the JWST and in the HST data, with the HST WFC3 data (F160W, corresponding to rest-frame B band; Zakamska et al. 2019) used as the background image. The gray outline roughly traces the [O III] emission shown in Wylezalek et al. (2022).
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: The same as Figure 8 but for Δn and n PT. The gray region denotes the range of parameters that cannot be reached or constrained by our model, due to our choice of performing the high-density matching at n = 10n 0.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Allowed values of Δϵ and ϵ PT for PTs that either complete in stable NSs (top panel) or destabilize the NS sequence (bottom panel) when matching to the Komoltsev & Kurkela (2022) region at n = 10n 0. The green pluses denote the twin solutions, and the remaining markers show the parameters corresponding to EOSs studied in the literature (see Table 1). The dashed red line denotes the 99.5% confidence contour when matching to the Annala et al. (2022) region at n = 10n 0.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Locations of the PTs (each drawn as a line with a random color) in our ensemble matched to the maximal n = 10n 0 region from Komoltsev & Kurkela (2022) shown in salmon color. Top panel: EOSs for which the PT completes within the stable NS sequence, with twin solutions shown in green. Note that for most of the twin solutions, the central densities occur at much higher densities than the ends of the PTs. Bottom panel: EOSs for which the PT destabilizes the NS sequence.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Top panel: region of allowed central ϵ and p points along the stable NS sequence with twin-star configurations removed, when using the more general n = 10n 0 matching region of Komoltsev & Kurkela (2022; shown in salmon color), after imposing the two astrophysical constraints M TOV > 2M ⊙ and ﹩{\tilde{{\rm{\Lambda }}}}_{\mathrm{GW}170817}\lt 720﹩. Bottom panel: individual p–ϵ sequences corresponding to the twin-star solutions, with the unstable branches shown in light gray.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Top panel: correlation of R (1.4M ⊙) and Λ (1.4M ⊙), divided into EOSs with transition densities n PT < 2n 0 (blue) and n PT ≥ 2n 0 (red). The overlap of these regions is shown in blended color. Bottom panel: correlation of Λ (1.4M ⊙) with the transition density n PT, with the points colored by their R (1.4M ⊙) values. Note that the largest-radius stars exhibit early PTs.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Range of allowed ϵ and p values at 10n 0. The cyan region corresponds to that shown in Figure 1, while the salmon one is the more general n = 10n 0 matching region of Komoltsev & Kurkela (2022). The points denoted by “causality” correspond to our construction prior to applying astrophysical constraints.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: The maximum possible mass of the core of high-density matter for EOSs with different PT parameters. Also shown are white contour lines of constant core masses (in units of M ⊙) to make details of the small-core-mass region more visible. Here, only points leading to nonzero core masses are shown.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: Top panel: region of allowed masses and radii when matching to the Komoltsev & Kurkela (2022) region at n = 10n 0, with twin-star configurations removed. Bottom panel: M–R sequences corresponding to the individual twin-star solutions, with the unstable branches shown in light gray.
Paper: Constraints on Strong Phase Transitions in Neutron Stars
Authors: T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, A. Vuorinen
Figure caption: The mass fraction of the core ﹩{M}_{\mathrm{core}}/M﹩ for different cuts on Δn/n. Note that the cuts shown correspond to the red lines in Figure 10.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: CDFs of the CNM, WNM, CNM+WNM column density, CNM fraction, and CNM component density. As in Figure 6, the four groups are shown in different colors and line styles: CO non-detection (thick solid gray), CO detection (thin solid black), Case A (thick dashed blue), and Case B (thin dashed tan). The column densities of Cases A and B are lower than those of the CO non-detection and detection by design (integrated over smaller velocity ranges) and are shown here only for the sake of completeness.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Comparison between the S14-based total number densities (﹩{n}^{\exp };﹩ gray circles) and the observationally inferred CNM densities (﹩{n}_{\mathrm{CNM}}^{\mathrm{obs}};﹩ blue squares) as a function of the CNM column density for the 19 CO-detected LOSs. Since the predicted ﹩{n}^{\exp }﹩ corresponds to the total gas number density (n 1 + 2n 2) at which H2 formation is expected to occur, it should be higher than ﹩{n}_{\mathrm{CNM}}^{\mathrm{obs}}﹩. Finally, the observed variation in the thermal pressure, log10(P/k B cm−3 K) = 3.58 ± 0.18, is indicated as the 1σ error bars for ﹩{n}_{\mathrm{CNM}}^{\mathrm{obs}}﹩. (Top) Entire LOS. (Middle) Case A. (Bottom) Case B.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Possible distributions of the WNM, CNM, and CO (tan, blue, and black, respectively). Based on our finding of the kinematic association between H I and CO (Section 6.1), the WNM is represented as the diffuse background, while the CNM and CO are shown as the smaller embedded structures. The velocities of the CNM and CO are indicated as blue and black arrows with arbitrary sizes, and UV radiation is presented as yellow arrows. (Left) Scenario for the Entire LOS, where CNM components at different velocities belong to one large structure and contribute to the shielding of the CO core. (Right) Scenario for Cases A and B, where CNM components close to CO only provide shielding against UV radiation.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: CDFs of the spin temperature, optical depth, CNM and WNM column density. In each panel, the four groups are shown in different colors and line styles: CO non-detection (thick solid gray), CO detection (thin solid black), Case A (thick dashed blue), and Case B (thin dashed tan).
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: CDFs of the spin temperature, optical depth, CNM and WNM column density. All H I components toward LOSs at b < −5° from the GNOMES and ALMA-NOEMA/21-SPONGE surveys are shown in thin black and thick gray (solid lines). Among these components, those in close proximity to CO and HCO+ in velocity are selected and presented in thin tan and thick pink (dashed lines).
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: CO peak brightness temperature as a function of Planck-based A  V . The 19 CO-detected LOSs are shown in tan, while upper limits based on 3σ values are indicated as downward arrows for the 39 CO non-detected LOSs.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: CDF of the absolute velocity difference between H I and CO (CNM and CO in thick blue; WNM and CO in thin tan). For these CDFs, H I components that are closest to the observed CO emission in velocity were considered.
Paper: Probing the Conditions for the H I-to-H2 Transition in the Interstellar Medium
Authors: Gyueun Park, Min-Young Lee, Shmuel Bialy, Blakesley Burkhart, J. R. Dawson, Carl Heiles, Di Li, Claire Murray, Hiep Nguyen, Anita Hafner, Daniel R. Rybarczyk, Snežana Stanimirović
Figure caption: Comparison between the H I absorption (thin blue) and CO emission (thick gray) spectra toward the 19 CO-detected LOSs. The spectra are aligned at peaks for ease of comparison.
Paper: In Search of Infall Motion in Molecular Clumps. IV. Mapping of the Global Infall Sources
Authors: Yang Yang, Xi Chen, Zhibo Jiang, Zhiwei Chen, Shuling Yu, Jun Li
Figure caption: Left: an example of the HCO+ (1–0) map grid of target G037.05-0.03 (gridded to half of the beam size). The axes plot the offsets ΔR.A. and Δdecl. relative to the coordinates from Table 1. Right: an HCO+ and H13CO+ map grid that enlarges the red boxed area of the left panel. The gas infall velocity and its uncertainty (in parentheses) are marked in each grid.
Paper: In Search of Infall Motion in Molecular Clumps. IV. Mapping of the Global Infall Sources
Authors: Yang Yang, Xi Chen, Zhibo Jiang, Zhiwei Chen, Shuling Yu, Jun Li
Figure caption: The spatial distribution maps of the infall velocity (the left panel of each subfigure) and images of the variation in infall velocity with distance to the clump center and the H13CO+ integrated intensity (the right panels of each subfigure, from top to bottom). The contours (gray) are the H13CO+ integrated intensity values of each source. For the sources without H13CO+ emissions detected, the integrated intensity of HCO+ is used. The red plus sign marks the position of the clump center in each velocity distribution map. The red dotted line represents the regression line of the two variables in the right panel of each subfigure.
Paper: In Search of Infall Motion in Molecular Clumps. IV. Mapping of the Global Infall Sources
Authors: Yang Yang, Xi Chen, Zhibo Jiang, Zhiwei Chen, Shuling Yu, Jun Li
Figure caption: Example of target G037.05-0.03: HCO+ (1–0) and H13CO+ (1–0) integrated intensity maps. The contours (blue) mark [0.2, 0.4, 0.6, 0.8] of the maximum value of its integrated intensity. The pentagram symbol denotes the position of the infall candidate identified in Paper II. The green, yellow, and orange points denote the Class I, flat-spectrum, Class II YSOs, respectively. The magenta crosses denote the 6.7 GHz methanol masers. The black circles at the lower left indicate the beam size of the IRAM 30 m telescope.
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: 1D marginalized posterior distributions and 2D 1-2σ contour regions for H 0 and/or Ωm. The colors represent: ΛCDM with a flat prior Ωm ∈ [0,  1] (red), ΛCDM with a Gaussian prior Ωm = 0.315 ± 0.007 (green), and R h = ct (blue).
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: 1D marginalized posterior distributions and 2D 1–2σ contour regions for the cosmological parameters H 0, Ωm, and/or ΩΛ, using the simulated sample with 1150 FRBs, assuming ΛCDM as the background cosmology. The colors represent: the best-fit nonflat ΛCDM (red contours) and R h = ct (blue line).
Paper: In Search of Infall Motion in Molecular Clumps. IV. Mapping of the Global Infall Sources
Authors: Yang Yang, Xi Chen, Zhibo Jiang, Zhiwei Chen, Shuling Yu, Jun Li
Figure caption: The average spectra of HCO+ (1–0) and H13CO+ (1–0) over the entire mapping area. The green lines show the results of Gaussian fitting of H13CO+ (1–0), and the dashed red lines indicate the central radial velocity of H13CO+ (1–0) (if H13CO+ emissions are not detected, we use C18O data to trace the central radial velocity).
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: Same as Figure 3, except now using the simulated sample with 550 FRBs, assuming R h = ct as the background cosmology.
Paper: Investigating Cosmological Models and the Hubble Tension Using Localized Fast Radio Bursts
Authors: Jun-Jie Wei, Fulvio Melia
Figure caption: The inferred upper limit of H 0 as a function of Ωm.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Left: the NIR SED of S5-z17-1. The red circles and arrows indicate the observed flux densities and 2σ upper limits, respectively. The blue and green curves and redshift labels represent the best-fit model SEDs and photometric redshifts by CIGALE with the redshift range at 0 < z < 25 and 0 < z < 10, respectively. The blue and green open circles are predicted flux densities in the NIRCam filters based on the best-fit SEDs. The low-z forced SED has a brighter submillimeter flux by >100 times than the best-fit high-z SED, expecting a ∼10σ detection from the ALMA Band 7 observation (gray curve in Figure 3). The images on this panel present 2″ × 2″ NIRCam cutout images of S5-z17-1. Middle: P(z) from the SED fitting by EAZY (brown curve) and CIGALE (light blue curve) with a redshift range at 0 < z < 25. Right: same as the middle panel, but at 0 < z < 10. The gray dashed line denotes the atmospheric transmission for [C II]. The red shade indicates the [C II] redshift range of z = 4.31–4.69 covered by our ALMA Band 7 observations spanning 334–358 GHz with three frequency tunings, which is optimized to maximally cover the peak of the lower-redshift solution’s P(z) and avoid the significantly low atmospheric transmission.