adsabs/AstroCLIMB huggingface dataset:
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The magnetograms of AR 13751 from the FMG, HMI_cropping, and SHARP data. AR 13751 produced an M-class flare at 10:00 UTC on 2024 July 18.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The architecture of the MViT flare prediction model.
Paper: Intelligent Forecasting for Solar Flares Using Magnetograms from SDO/SHARP, SDO/HMI, and ASO-S/FMG
Authors: Xuebao Li, Hongwei Ye, Yanfang Zheng, Ting Li, Jiaben Lin, Shunhuang Zhang, Pengchao Yan, Yongshang Lv, Noraisyah Mohamed Shah, Xuefeng Li, Xiaotian Wang, Yingbo Liu, Rui Wang, Jinfang Wei, Changtian Xiang, Honglei Jin
Figure caption: The architecture of the ViT flare prediction model.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Characteristics of same plasma parcel, highlighted by the cyan shadows, observed on 2022 December 10 by PSP (left column) and on 2022 December 15 by SO (right column). Panels from top to bottom show the magnetic field magnitude B, component of magnetic field vector in RTN coordinates Brtn, proton density Np, radial component of solar wind speed Vr, cosine of the angle between the magnetic field and velocity field vectors cos θBV, plasma beta β, and normalized cross-helicity σc. The vertical black dashed line in each column indicates the model-predicted time tin at PSP and tout at SO, corresponding to the same plasma parcel.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Plasma propagation considering a constant acceleration a. Panel (a) shows the color map of ﹩{\rm{\Delta }}V=\left\langle {V}_{\rm{p, SO}\,}\right\rangle -{V}_{\,\rm{out}}﹩, where the minimum of ﹩\left|{\rm{\Delta }}V\right|﹩ is indicated by the black curve. Panel (b) shows values of Vin (blue curve), calculated as averages of Vp, PSP over a 1 hr interval centered on tin, ﹩\left\langle {V}_{\,\rm{p, SO}\,}\right\rangle ﹩ (orange curve) and Vout (green curve) given by Equation (7). Panel (c) shows the minimum distance dmin corresponding to the radial acceleration for minimum of ﹩\left|{\rm{\Delta }}V\right|﹩. Panel (d) shows the corresponding propagation times τ (in black) and tout (in green). All quantities are shown as a function of tin.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Local comparison of the plasma parcel observed by both PSP and SO by scaling PSP-measured proton density Np and magnetic field magnitude B with a factor R−2 and R−1.8, respectively, to take the adiabatic expansion from PSP (blue) to SO (orange) into account.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Positions of PSP and SO relative to the Sun for the studied radial alignment event. Panel (a) shows the trajectories of PSP (blue curve) and SO (red curve) in the X–Y plane of the ECLIPJ2000 coordinate system during the period of 2022 December 3–17. The black dashed line indicates the radial line from the Sun passing through the PSP and SO at the alignment time t0 ∼ 02:00 UT on 2022 December 10. Blue squares and red triangles indicate the positions of PSP and SO at three different instants in time, respectively. The green circle along each spacecraft’s trajectory denotes the approximate crossing time of the same plasma parcel during this alignment. Panels (b) and (c) display the latitude (θ) and longitude (ϕ) of PSP and SO, respectively. The black vertical dashed line marks the spacecraft alignment time t0.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Pearson’s cross-correlation coefficient for proton density Np (black curve) and the magnetic field magnitude B (red curve) between PSP and SO measurements.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Helium abundance as the He/H number density ratio for PSP (left) and SO (right). The black points show the spacecraft-observed values, while red solid curves represent the 50 point median filter. Large circles with error bars represent mean values with 1σ uncertainty within the shaded interval.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: PFSS model for PSP on 2022 December 10 05:00 and SO on 2022 December 15 02:30 using an input ADAPT-GONG magnetogram.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Power spectral density (PSD) of the total magnetic field fluctuations, separated into compressible parallel (P∥, pink solid lines) and transverse fluctuations (P⊥, green solid lines) (panels (a) and (b)), and magnetic compressibility CB (panels (c) and (d)) for the intervals observed by PSP (left column) at 0.11 au and SO (right column) at 0.88 au. The best power-law fits are represented by dashed lines in the respective colors, and the corresponding spectral break frequency fb is indicated by a black arrow. The vertical dashed lines indicate the proton gyrofrequency fp in the plasma frame.
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Top panels: Comparison of reconstructed structure functions for PSP (panel (a)) and SO (panel (b)) intervals, based on the fitted parameters μ(τ) and λ2(τ) of the Castaing function (colored lines, corresponding to different orders, q), with observational results (black circles). The structure functions are shown for orders q = 0.5, 1.0, 1.5, 2.5, 3.0, and 3.5. The vertical blue dashed lines indicate the fitting range of the structure functions used to determine the scaling exponent. Bottom panels: Scale dependence of flatness for PSP (panel (c)) and SO (panel (d)) intervals. Black lines represent flatness from observational data, while red lines correspond to values derived from the Castaing parameter λ2(τ).
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: Scaling exponent of the structure function vs. order q in the MHD inertial range for PSP (panel (a)) and SO (panel (b)) intervals. The scaling exponents ζ(q), shown in black curves, are obtained from the power-law fit of data with ﹩{S}^{q}(\tau )\sim {({S}^{2}(\tau ))}^{-\zeta (q)/\zeta (2)}﹩, while the red curves represent the theoretical scaling exponent ζ(q) obtained on the basis of Castaing function using Equation (12).
Paper: Evolution of Solar Wind Turbulence during Radial Alignment of Parker Solar Probe and Solar Orbiter in 2022 December
Authors: Ashok Silwal, Lingling Zhao, Xingyu Zhu, Luca Sorriso-Valvo, Lina Z. Hadid, Gary P. Zank, Hui Li, Samuel T. Badman, Yeimy J. Rivera, Sujan Prasad Gautam, Monika Karki, Juan G Alonso Guzman, Nibuna S. M. Subashchandar, Zeping Jin
Figure caption: PDFs of magnetic field increments at three different timescales (τ; see legends) for the radial (δBr; top row), tangential (δBt; middle row), and normal (δBn; bottom row) components. A Gaussian distribution is shown as a reference (dashed black line).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: ALMA footprints overlaid on the NIRCam RBG (R: F444W, G: F356W, B: F277W) map of A2744 taken in UNCOVER (R. Bezanson et al. 2024). The yellow solid curve shows the relative sensitivity response to the deepest 20% of the mosaic of DUALZ, matched to the NIRCam footprint of the UNCOVER survey, and the green and cyan dashed curves present those of ALMA-HFF (A. M. Muñoz Arancibia et al. 2023) and ALCS (S. Fujimoto et al. 2024a). The white-shaded region indicates the highly magnified area with magnifications of ≥2 (L. J. Furtak et al. 2023a).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: RGB NIRCam color cutouts (8″ × 8″) for the 69 ALMA sources identified in the survey (R: F444W, G: F277W, B: F150W). The green and magenta contours represent the 3σ, 4σ, and 5σ significance levels of the ALMA 1.2 mm continuum in the natural and tapered maps, respectively, with the map showing the higher SNR being adopted. The white contours denote the −3σ, −4σ, and −5σ significance levels. The ellipse displayed at the bottom right represents the ALMA synthesized beam.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Example of the 2D (top) and 1D (bottom) JWST/NIRSpec prism spectra taken for the ALMA sources in DUALZ. The inset panel shows the NIRCam RBG 5″ × 5″ cutout, where the three shutter positions are overlaid. The inset label shows the MSA ID and our best-fit redshift estimate from the prism spectrum. To avoid self-subtraction, we use the global background subtraction for the 2D and 1D spectra instead of the standard three shutter-nod method for this source in this paper (see the text). The red and magenta curves (horizontal dashed lines) in the bottom (top) panel indicate the 1D spectra (extraction apertures) for the data taken from the shutters highlighted with the red and magenta rectangles in the inset panel, respectively. The black vertical lines denote wavelengths of the emission lines detected at SNR ≥ 4.0. The Balmer decrement via Paγ/Paβ shows the spatial variation of the dust attenuation, demonstrating the power of NIRSpec MSA also in the spatially resolved fashions.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: RGB NIRCam color cutouts (5″ × 5″) for the eight HST-dark ALMA sources, selected with the color–magnitude criteria (Figure 9). For the selection, we use the ﹩0\mathop{.}\limits^{^{\prime\prime} }32﹩-diameter aperture photometry in NIRCam to fairly investigate the NIR color properties in the compact dust-emitting regions, and thus, the outer regions are clearly visible in HST/F160W in some cases. Using the intrinsic magnitude after the magnification correction may also make some sources clearly visible in HST. The RGB filter assignment is identical to Figure 6. Green contours represent the 3σ, 4σ, and 5σ significance levels of the ALMA 1.2 mm continuum in the natural map. The red cross and its bar scale indicate the ALMA peak pixel position and its positional uncertainty, calculated based on the ALMA beam size and SNR (see the text). The ellipse displayed in the bottom panel represents the ALMA synthesized beam. The brown circle denotes the ﹩0\mathop{.}\limits^{^{\prime\prime} }32﹩-diameter aperture used for the NIRCam photometry (J. R. Weaver et al. 2024).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Survey area against the limiting 1.2 mm flux (S1.2mm,limit; 5σ) for DUALZ and other large ALMA surveys in the literature (J. González-López et al. 2020; C. M. Casey et al. 2021; C. Gómez-Guijarro et al. 2022; A. M. Muñoz Arancibia et al. 2023; S. Fujimoto et al. 2024a). For the lensing cluster studies, the lens correction is applied assuming z = 2.0.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Differential counts of positive (red) and negative (blue) sources as a function of peak SNR. From left to right, we present the results obtained from the Wide-natural, Wide-tapered, Deep-natural, and Deep-tapered maps. The vertical dashed line denotes the SNR threshold adopted in this paper for each map, to reliably identify ALMA sources in a blind manner.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Color–magnitude diagram (F150W vs. F150W-F444W). Filled and open green circles denote our ALMA sources before and after lens correction, respectively. Filled and open red circles indicate the eight ALMA sources whose colors meet the selection criteria (red dashed line; F150W > 27 mag, F150W-F444W > 2.3 mag) of the HST-dark galaxies, similar to the method of L. Barrufet et al. (2023). Black circles represent the NIRCam sources detected in UNCOVER (J. R. Weaver et al. 2024).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: ALMA Band 6 continuum mosaic maps without primary beam correction (left) and relative sensitivity response maps of the mosaic (right) of DUALZ-wide (top panels) and DUALZ-deep (bottom panels). The DUALZ-wide mosaic was accomplished by combining the four mosaics of A, B, C, and D labeled on the top-right panel. The labeled green circles represent the ALMA continuum sources. The white lines denote the μ = 200 magnification curve at z = 6. The white square indicates the footprint of the ALMA-HFF, inside of where we use the DUALZ-deep map to complementary identify further faint ALMA sources.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Comparison between zphot and zspec for the spec-z confirmed 27 ALMA sources identified in the DUALZ survey. All 27 sources fall in ∣zspec − zphot∣/(1 + zspec) < 0.15.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Sensitivity (PB = 1.0) of the Wide-natural and Deep-natural data cube. The previous data covers 250–257.5 GHz and 265–272.5 GHz, where the sensitivity of the deep cube is better than that of the Wide cube by a factor of ∼3.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: IRLF measurements out to z ∼ 10. The red-filled circles represent our DUALZ measurements. The red open circles indicate the possible constraints from the two JWST-dark ALMA galaxy candidates (Section 4.2.2) and the marginal (∼2.6σ) ALMA detection from the X-ray AGN at z = 10.07 (Section 4.4) if they are real. The red open square denotes the marginal (∼2.3σ) ALMA detection in the stacked image of the 16 NIRCam sources at z ≳ 9 presented in Figure 15. Our measurements do not include completeness correction. Previous IRLF measurements with Herschel (C. Gruppioni et al. 2013; B. Magnelli et al. 2013; F. Wang et al. 2019a) ALMA+SCUBA2 (M. P. Koprowski et al. 2017), and ALMA (B. Hatsukade et al. 2018; U. Dudzevičiūtė et al. 2020; C. Gruppioni et al. 2020; S. Fujimoto et al. 2024a) are shown in gray and other colored symbols, together with the best-fit DPL function estimated in J. A. Zavala et al. (2021) and S. Fujimoto et al. (2024a). The other color lines show the predictions from simulations (M. Béthermin et al. 2022; C. d. P. Lagos et al. 2020; J. W. Trayford et al. 2020; A. P. Vijayan et al. 2022; V. Mauerhofer & P. Dayal 2023), where the turnover in the faint IR luminosity range in some of these simulations is caused by the incompleteness due to the mass resolution limit in their calculations. The gray bar represents the increase of the LIR at z = 9 with increasing Td assumption.