adsabs/AstroCLIMB huggingface dataset:
Paper: Simulating X-Ray Reverberation in the Ultraviolet-emitting Regions of Active Galactic Nuclei Accretion Disks with Three-dimensional Multifrequency Radiation Magnetohydrodynamic Simulations
Authors: Amy Secunda, Yan-Fei Jiang, 燕飞 姜, Jenny E. Greene
Figure caption: The top panels show the PSDs of the intrinsic UV, reprocessed UV, and injected X-ray light curves in Figure 2. The bottom panels compare the PSDs of the injected and emitted X-rays. The left (right) panels show the PSDs from Run A (Run B), where τ damp = 30 days (τ damp = 0.1 day) for the injected X-ray light curve. We see some evidence that the UV PSDs are damped at f ≲ 0.03 day−1. At 0.03 < f < 0.2 day−1, the slope of the UV PSDs appear to be well fit by f −2, shown as the dashed line, which is the DRW slope above the damping frequency. At f > 0.2 day−1, the UV PSDs are well fit by f −2.5, shown as the dotted line.
Paper: New Light on Dark Extended Lenses with the Roman Space Telescope
Authors: William DeRocco, Nolan Smyth, Volodymyr Takhistov
Figure caption: Projected sensitivity to different extended lenses. Solid lines are estimates for 72 day seasons. The dashed lines show the projected sensitivity to R 90 = 0.1 R ⊙ lenses using 60 day seasons. Existing limits from Subaru, OGLE, and EROS are shown in shaded regions (Croon et al. 2020b) with the color corresponding to the extent of the lens. The gray shading corresponds to limits on pointlike lenses with mass M dPBH ≈ 100 M PBH, corresponding to the most optimistic current constraints on dressed PBH (see Cai et al. 2023 for details).
Paper: New Light on Dark Extended Lenses with the Roman Space Telescope
Authors: William DeRocco, Nolan Smyth, Volodymyr Takhistov
Figure caption: Representative lightcurves for the three extended lens species (colored lines) plotted alongside a point lens (dotted line), all in the point-source regime. For certain parameter choices, the extended lenses can produce caustic features, seen here in the case of the NFW subhalo (blue) and axion/boson star (green). See the discussion below Equation (9).
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: The Δ[Fe/H]/Δ∣Z∣ as a function of the R for the thin (left panel) and thick (right panel) disks. The red dashed lines are the best fit of the global profiles of trends of Δ[Fe/H]/Δ∣Z∣–R.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: XRT light curve for Swift J010902.6-723710 from 2023 August to present, combining data from S-CUBED observations and follow-up targets of opportunity (TOOs). Note source visibility to Swift is indicated by the gray background, white vertical strips indicate periods when the target could not be observed. Vertical dotted lines mark predicted times for the periastron passages.(The data used to create this figure are available.)
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: The vertical metallicity gradient with the subtracted fitted profile in Figure 4, Cor Δ[Fe/H]/Δ∣Z∣ (defined as Δ[Fe/H]/Δ∣Z∣ − Fit_Δ[Fe/H]/Δ∣Z∣), as a function of R, for thin (left panel) and thick (right panel) disks. The red lines are the best fit with Equation (1).
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption:                       ﹩{Z}_{2}^{2}﹩ periodogram for four observations with exposures of ≃5 ks of Swift XRT data taken in PC mode. The periodogram shows a peak at 182 s in all four observations made after outburst was detected by S-CUBED weekly monitoring. There is evidence for pulsar spin-up over time; however, the errors on period measurement are large, meaning this result is not statistically significant.
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: The [Fe/H]−[α/Fe] distribution of the LAMOST-APOGEE RC stars, color-coded by the logarithmic number densities and overplotted with contours of equal densities. The [Fe/H] and [α/Fe] axes are spaced by 0.025 dex and 0.02 dex, respectively. There is a minimum of 20 stars per bin. The two dashed lines are used to separate the thin (below the lines) and thick (above the lines) disks.
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: The relative distance error (Δs, defined as the ratio of the distance error σ d to distance d) as a function of R. The red line is the best fit for the whole RC sample stars.
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption:  α 0 as a function of R for thin (left panel) and thick (right panel) disks. The red lines are the best fit with Equation (5).
Paper: On the Chemical and Kinematic Signatures of the Resonances of the Galactic Bar as Revealed by the LAMOST-APOGEE Red Clump Stars
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: Spatial distribution of the LAMOST-APOGEE RC stars in the R–Z plane, color-coded by the stellar number densities. Both axes are spaced by 0.1 kpc, with no less than eight stars in a bin.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: Detrended OGLE data divided into five consecutive epochs (see Table 1) and each then folded using the ephemeris given in Equation (1). For the purpose of being able to see the separate profiles, those numbered 2–4 have been arbitrarily shifted in the y-axis such as to avoid overlap.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: Corbet diagram for all BeXRBs in the SMC with known orbital periods and spin periods (Haberl & Pietsch 2005; Coe & Kirk 2015; Carpano et al. 2017; McBride et al. 2017; Kennea et al. 2018, 2020; Lazzarini et al. 2019; Carpano et al. 2022; Maitra et al. 2023). SXP 182 is plotted alongside these data and is shown to demonstrate the same correlation between X-ray pulsar spin period and NS orbital period that is seen in the rest of the SMC BeXRB population.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: The evolution of the Hα emission line from SALT observations. The spectra are corrected for the heliocenter and redshift of the SMC.(The data used to create this figure are available.)
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: A comparison of the OGLE IV and UVOT light curves folded at the proposed binary period of 60.623 days using Equation (1). The OGLE data are offset vertically to avoid overlap.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: The SALT spectrum of Swift J010902.6-723710 covering the blue region with different line species labeled at their expected rest wavelengths. The spectrum is corrected for the heliocenter and redshift of the SMC.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: OGLE IV, Swift UVOT, and Swift XRT light curves for Swift J010902.6-723710.(The data used to create this figure are available.)
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: (V − I) − I (left) and (U − I) − I (right) color–magnitude diagrams of Swift J010902.6-723710.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: Top panel—the whole OGLE data set covering 26 yr. Lower panel—the above data detrended with a simple polynomial in preparation for timing analysis.(The data used to create this figure are available.)
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: Generalized Lomb–Scargle analysis of the detrended OGLE data set. The peak is at a period of 60.623 ± 0.001 days. The horizontal dashed line represents the false alarm probabilty of 1%.
Paper: JWST MIRI MRS Images of Disk Winds, Water, and CO in an Edge-on Protoplanetary Disk
Authors: Nicole Arulanantham, M. K. McClure, Klaus Pontoppidan, Tracy L. Beck, J. A. Sturm, D. Harsono, A. C. A. Boogert, M. Cordiner, E. Dartois, M. N. Drozdovskaya, C. Espaillat, G. J. Melnick, J. A. Noble, M. E. Palumbo, Y. J. Pendleton, H. Terada, E. F. van Dishoeck
Figure caption: MIRI MRS images of Tau 042021, showing the ALMA 0.89 mm dust continuum (top left; Villenave et al. 2020) and emission lines from H2 S(2) 12.278 μm (top right), [Ne II] 12.814 μm (bottom left), and H I Humphreys α 12.372 μm (bottom right) detected with the MIRI MRS. White contours in each image show the mid-IR scattered-light continuum at 12.2 μm, and the white dashed lines show the position angle measured from the ALMA continuum image (PA = −16°; Villenave et al. 2020). Images have been scaled using an asinh stretch to maximize the contrast between the background noise and the high-S/N emission from the source. Beige circles in the bottom left corner of each panel represent the average theoretical FWHM of the PSF, calculated from the relationship reported in Law et al. (2023). The observed spatial distributions are consistent with micron-sized grains in the eastern and western reflection nebulae (12 μm continuum), a disk wind (H2 S(2)), a bipolar jet ([Ne II]), and scattered light from accretion shocks or from the base of the jet (H I). We note that the position angle of the jet is tilted by ∼2.°5 relative to the disk.
Paper: JWST MIRI MRS Images of Disk Winds, Water, and CO in an Edge-on Protoplanetary Disk
Authors: Nicole Arulanantham, M. K. McClure, Klaus Pontoppidan, Tracy L. Beck, J. A. Sturm, D. Harsono, A. C. A. Boogert, M. Cordiner, E. Dartois, M. N. Drozdovskaya, C. Espaillat, G. J. Melnick, J. A. Noble, M. E. Palumbo, Y. J. Pendleton, H. Terada, E. F. van Dishoeck
Figure caption: MIRI MRS line images of Tau 042021, showing stacked emission lines from the CO v = 1 − 0 (left) and H2O v 2 = 1 − 0 transitions, detected with the MIRI MRS. White contours in each image show the mid-IR scattered-light continuum at 5.0 μm. Images have been scaled using an asinh stretch to maximize the contrast between the background noise and the high-S/N emission from the source. Beige circles in the bottom left corner of each panel represent the average theoretical FWHM of the PSF, calculated from the relationship reported in Law et al. (2023). The emission is spatially extended beyond the expected size of the inner disk, r < 1 au, consistent with scattering by micron-sized dust grains in disk surface layers (see, e.g., Duchêne et al. 2024).
Paper: JWST MIRI MRS Images of Disk Winds, Water, and CO in an Edge-on Protoplanetary Disk
Authors: Nicole Arulanantham, M. K. McClure, Klaus Pontoppidan, Tracy L. Beck, J. A. Sturm, D. Harsono, A. C. A. Boogert, M. Cordiner, E. Dartois, M. N. Drozdovskaya, C. Espaillat, G. J. Melnick, J. A. Noble, M. E. Palumbo, Y. J. Pendleton, H. Terada, E. F. van Dishoeck
Figure caption: Left: 1D MIRI MRS spectrum of Tau 042021, extracted from the eastern (top) and western (bottom) reflection nebulae. We detect H2 emission lines and forbidden emission lines from [Ne II], [Ne III], and [Fe II] on both sides of the disk. H2O and CO2 ice absorptions are also identified, along with PAH emission near 11 μm. Right: zoomed-in spectra of rovibrational CO, rovibrational H2O, and rotational H2O emission lines from the eastern reflection nebula, with LTE slab models overlaid in cyan (Salyk 2022). The CO model has a temperature and column density of T = 1500 K and ﹩\mathrm{log}N=17.5﹩ cm−2, and the rotational H2O emission lines are consistent with T = 850 K and ﹩\mathrm{log}N=15.0﹩. The rovibrational lines are shown with the rotational model scaled down by a factor of 20 in flux.
Paper: JWST MIRI MRS Images of Disk Winds, Water, and CO in an Edge-on Protoplanetary Disk
Authors: Nicole Arulanantham, M. K. McClure, Klaus Pontoppidan, Tracy L. Beck, J. A. Sturm, D. Harsono, A. C. A. Boogert, M. Cordiner, E. Dartois, M. N. Drozdovskaya, C. Espaillat, G. J. Melnick, J. A. Noble, M. E. Palumbo, Y. J. Pendleton, H. Terada, E. F. van Dishoeck
Figure caption: MIRI MRS image of 11.3 μm PAH emission, which is spatially colocated with the scattered-light continuum from Tau 042021. While PAH emission is readily detected in disks around more massive stars and in more externally irradiated environments (see, e.g., Geers et al. 2006, 2007), it is rare to detect the band within disks around M-type stars. We note that the continuum on the red side of the band is beyond the edge of the channel 2 detector, making it challenging to extract the total surface brightness profile. The image shown here is from a single frame where the feature peaks in emission.
Paper: JWST MIRI MRS Images of Disk Winds, Water, and CO in an Edge-on Protoplanetary Disk
Authors: Nicole Arulanantham, M. K. McClure, Klaus Pontoppidan, Tracy L. Beck, J. A. Sturm, D. Harsono, A. C. A. Boogert, M. Cordiner, E. Dartois, M. N. Drozdovskaya, C. Espaillat, G. J. Melnick, J. A. Noble, M. E. Palumbo, Y. J. Pendleton, H. Terada, E. F. van Dishoeck
Figure caption: Emission-weighted velocity maps of H2 S(2) (left) and [Ne II] emission lines from Tau 042021 (right; see, e.g., Beck et al. 2008; Narang et al. 2024). No velocity structure is detected in either of the maps, as expected for an edge-on disk from which the maximum jet and wind velocity components are not oriented along the line of sight.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Left: predicted cumulative number of high-redshift galaxies detected across the NGDEEP NIRCam imaging mosaic. Simulations (solid lines; Mason et al. 2015b; Behroozi & Silk 2015; Dayal et al. 2017; Wilkins et al. 2022, Yung et al. 2023) span a wide range, reflecting the lack of observational constraints prior to JWST. Across the full NGDEEP NIRCam mosaic (to the F277W 5σ limit) NGDEEP should cover ∼50–1100 galaxies at z ∼ 10, 3–25 galaxies a z ∼ 13, and up to 10 galaxies at z = 13.5–15, distinguishing between these models. We note that early results from CEERS (Finkelstein et al. 2023) are consistent with the most optimistic of these models (Behroozi & Silk 2015). Right: model uncertainties highlight our state of knowledge of important physical processes. Purple shading shows the plausible range of the dependence of SFR on gas surface density, which primarily affects the bright end, which is constrained by wider-area programs like CEERS and COSMOS-Web (Casey et al. 2023). Red shading denotes the plausible range in stellar feedback mass-loading factors, which primarily affect the faint end (Yung et al. 2019a). The symbols show the precision achievable by CEERS and NGDEEP+JADES (assuming the fiducial Yung et al. 2019a UVLF; dotted line). At M UV = −17.5 (NGDEEP-NRC 10σ limit), NGDEEP-NRC alone will significantly constrain these models (∼4.5σ, including cosmic variance, improving to ∼5.5σ with the eventual combination with JADES), placing the first definitive constraints on feedback processes in early galaxies.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: NGDEEP-NIS will enable the measurement of the SFR–stellar mass (SFMS) relation and its scatter at z = 1–2, for galaxies 10–100× fainter than previous surveys (e.g., MOSDEF). Left: the predicted SFMS relation for NGDEEP-NIS (small red circles). NIRISS will derive SFRs from Hα for galaxies to SFR   =  0.22 (0.040) M ⊙ yr−1 at z = 2 (z = 1). The Hα-derived SFR limits are well matched to the UV-derived SFRs from the HUDF ACS F435W imaging. The black solid line shows the SFMS relation at z = 2 (Tomczak et al. 2014), and the black dashed line is the extrapolation to logM */M ⊙ < 9. Right: the NGDEEP-NIS Hα/UV SFRs will measure the scatter in the SFMS relation. The data points show the scatter from the SFMS relation for galaxies above a given stellar mass. For NIRISS, we show the true scatter (red open triangles) compared to the measured scatter (large red filled triangles), which includes measurement errors. The difference in the scatter between UV and Hα SFRs provides a strong constraint on feedback in simulations: this is predicted to be strongest at the lower stellar masses (logM */M ⊙ < 9; see Sparre et al. 2017) probed by NGDEEP-NIS.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Left: the area covered in each NGDEEP-NRC filter as a function of 5σ depth measured for resolved sources. The solid lines denote the full survey (Epochs 1 and 2 covering both position angles), and the dashed line shows the depth and area coverage achieved in Epoch 1 (V3_PA = 70°) for F277W as an example. The dotted lines show the depths that will be achieved by the JADES deep-field observations in the HUDF once the survey is completed. While JADES covers a larger area, NGDEEP-NRC will go ∼0.5 mag deeper in F444W and ∼0.3 mag deeper in F115W, allowing for the detection of z > 9.5 Lyα breaks in galaxies at the detection limit in F150W, F200W, and F277W. As a treasury program, NGDEEP will also be public immediately, providing the community the opportunity to explore a JWST deep field right away in Cycle 1. Right: exposure time maps in 103 s for each of the six NGDEEP-NRC filters. The overlapping position angles, NIRISS filter FWHM-dependent direct imaging dithers, and short-wavelength detector gaps result in the multiple depth tiers that are present in the left panel.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Redshift vs. Hα flux for galaxies in simulated NGDEEP-NIS data. The small gray points represent all sources in the simulation. The red squares are simulated objects with NIRISS-detected Hα emission (S/N >3σ). NGDEEP will measure faint Hα emission from >900 sources from 0.7 < z < 2.3 (see Table 3). The open circles are sources that would have been targeted by MOSDEF, a dedicated survey using the 10 m Keck telescope. Surveys like MOSDEF must preselect objects and are subject to slit crowding: MOSDEF only targeted galaxies with H 160 < 25 AB mag and had a flux limit of F ≃ 10−17 erg s−1 cm−2 (3σ). MOSDEF would be sensitive to fewer than 70 of the NGDEEP-NIS sources (at higher stellar masses).