adsabs/AstroCLIMB huggingface dataset:
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Radial evolution of the number density n, radial velocity V  r , perpendicular temperature T ⊥, parallel temperature T ∥, and temperature anisotropy ﹩\tfrac{{T}_{\perp }-{T}_{\parallel }}{{T}_{\perp }+{T}_{\parallel }}﹩ for α-particles (left panels) and protons (right panels). The color bars on the right indicate the number of counts in each bin. The blue and red curves represent the local median value of the parameters for α-particles and protons, with the error bars indicating the quartiles of the local distributions. In panels (a), (b), (e), (f), (g), and (h), the median values are fitted with a power-law function and the result is depicted as black solid curves. The shaded regions in panels (e), (f), (g), and (h) display the model prediction using the double adiabatic theory to predict the radial evolution of perpendicular and parallel temperatures, assuming a proton flow speed in the range of 200–400 km s−1. For reference, temperature isotropy is indicated by the black dashed lines in panels (i) and (j).
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption:                       ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩-﹩\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}﹩ distributions as a function of V pr and ﹩\tfrac{\delta B}{{B}_{0}}﹩. (a) and (b) the horizontal axis is the proton velocity V pr, the vertical axis is the dimensionless drift speed ﹩\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}﹩, and the colors indicate ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩. (c)–(f) The horizontal axis is ﹩\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}﹩, and the vertical axis is ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩. The colors in (c) and (d) indicate the proton velocity V pr. The black dashed curves represent isocontours of constant maximum growth of the FM/W instability in terms of ﹩\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}﹩, the same as Figure 4. The colors in (e) and (f) indicate the ratio of the magnetic field perturbation standard deviation to the background magnetic field, where PSP uses magnetic field data over 30 minutes to calculate the magnetic field perturbation standard deviation, and Helios uses data over 40 s.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Radial evolution of (a) ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ and (b) ﹩\left|{V}_{\alpha p}\right|﹩. The black solid curve represents the local median while the error bars indicate the local quartiles. The blue solid curve and blue dashed curve illustrate the results from our model given by Equations (18) and (27), which predict ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ and V  α p  based on the median and quartiles of ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ and ﹩\left|{V}_{\alpha p}\right|﹩ at 0.357 au (the rightmost error bars). (b) The red dashed line with the arrow indicates the estimated outer boundary of the preferential acceleration zone.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Distribution of data in (β  p∥, V  α p ) space. The three rows represent the results from PSP, Helios within 0.5 au, and Helios beyond 0.5 au, respectively. From left to right, the four columns represent the number of counts in each bin, the bin-averaged temperature ratio, the bin-averaged α-particle temperature anisotropy, and the bin-averaged proton temperature anisotropy. For the last three columns, the color saturation represents the ratio of the count number to a threshold count number (C 0), with C 0 = 100 for PSP data and C 0 = 10 for Helios data.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Radial evolution of Coulomb collision number N C and proton radial velocity V pr. Data from PSP and Helios both indicate that as V pr increases, N C decreases. Most of the V pr detected by PSP is less than 500 km s−1, while Helios detects a majority of wind streams with speeds greater than 500 km s−1.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Temperature anisotropy of α-particles and protons in V pr–N C space. (a) and (c) present PSP data, while (b) and (d) show Helios data. The color bar indicates the ratio of ﹩\tfrac{{T}_{\perp }}{{T}_{\parallel }}﹩.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Three-color images, with Spitzer SAGE 8 μm in red, Spitzer SAGE 24 μm in blue (M. Meixner et al. 2006), and Hα in green (R. C. Smith 1998). North is up; east is left. (a) Large-scale, three-color image of the LMC. (b) Zoomed-in three-color image of N77, N79, N81, and N83 identified by K. G. Henize (1956). N79, N83, and N77 have also been referred to as N79 South, N79 East, and N79 West in B. B. Ochsendorf et al. (2017), respectively. Two Spitzer-identified clusters of young stellar objects (YSOs) within N79 are circled in yellow (the location of H72.97–69.39) and magenta, known as N79S1 and N79S2, respectively (O. Nayak et al. 2024). The green box surrounding N79 is the field of view of the Chandra ACIS-I observations. (c) Zoomed-in three-color image of N79. The yellow box indicates the area surrounding H72.97-69.39 as shown in panel (d). (d) Zoomed-in three-color image in the vicinity of H72.97–69.39 (black cross).
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: X-ray images of H72.97–69.39 in soft [0.5 − 1.2 keV] (a), medium [1.2−2.0 keV] (b), hard [2.0−7.0 keV] (c), and broad band [0.5−7.0 keV] (d). The scale bar is 5″ ≈1.2 pc, and the images are 1﹩{}^{{\prime} }﹩ × 1﹩{}^{{\prime} }﹩ in size. A gray circle marks the position of H72.97–69.39, and five YSOs identified by O. Nayak et al. (2024) with JWST MRS data are labeled with cross symbols. North is up; east is left. The X-ray emission is extended ≈10″ and peaks ≈5″ offset from the position of H72.97–69.39.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Comparison of the (a) 13CO emission observed with Atacama Large Millimeter/submillimeter Array in red by O. Nayak et al. (2019) with the (b) DeMCELS Hα emission from S. D. Points et al. (2024) in green and (c) Chandra broadband (0.5−7.0 keV) X-ray emission in blue. The five YSOs identified with JWST by O. Nayak et al. (2024) are marked with crosses in panel (d). H72.97–69.39 is denoted by a magenta circle in all panels. The diffuse X-rays appear to fill the low-density cavities where 13CO is dim. Annuli in panel (c) were used to produce the multiband surface-brightness profiles in Figure 5. All images are 0.′75 × 0.′75 in size, and the scale bar is 5″ ≈ 1.2 pc at the distance of the LMC.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Background-subtracted surface-brightness profile (in units of net counts per square pixel) of the soft (red), medium (green), and hard (blue) X-ray bands for the three annuli in Figure 4(a). The hard X-rays have the greatest surface brightness near H72.97–69.39, and the medium and hard X-rays have comparable surface brightnesses at radii ≳2.4 pc. The soft X-rays are not statistically significantly detected in any annulus.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Zoomed-in Chandra ACIS-I images showing the source region (yellow diamond) and background regions (magenta diamonds) used to create spectra of H72.97–69.39. Each region is 1﹩{}^{{\prime} }﹩ × 1﹩{}^{{\prime} }﹩. The distance from the center of the source region to the center of the left-hand background region is ≈6.0﹩{}^{{\prime} }﹩ (≈87.5 pc), and the distance to the right-hand background region is ≈6.7﹩{}^{{\prime} }﹩ (≈98.1 pc). Panel (a) shows the soft [0.5−1.2 keV] X-ray band in red, panel (b) shows the medium [1.2−2.0 keV] in green, panel (c) shows the hard [2.0−7.0 keV] in blue, and panel (d) shows the broad band [0.5−7.0 keV] in orange.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Three-color X-ray image of N79S2, where the soft X-rays (0.5−1.2 keV) are in red, medium X-rays (1.2−2 keV) are in green, and hard X-rays (2−7 keV) are in blue. The three YSOs identified with the JWST MRS data from O. Nayak et al. (2024) are labeled. The hard X-rays dominate this source, likely because of the high-absorbing column in the direction of it. The image is 0.′75 × 0.′75; the scale bar is 5″ ≈ 1.2 pc at the distance of the LMC.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Line complex fitting for obtaining spectroscopic redshifts of candidate S-UMGs in the COSMOS field. For objects with confirmed redshifts, the regions of the 1D and 2D spectra with the confirming lines and fitted model are shown. The overall model is shown in red, while individual line components are shown in different colors (Hα in orange, [N II] λλ6548, 6584 in purple, and [S II] λλ6718, 6733 in magenta). For objects without confirmed redshifts (e.g., COS-DR1-79837, top right), the entire wavelength range probed by H- and K-band spectroscopy is shown. Some targets were observed with multiple masks which were sensitive to different wavelengths; in such cases regions covered by fewer than the total number of masks are displayed as a lighter shade of gray. Similar plots for the targeted S-UMG candidates in the VIDEO fields are in the Appendix.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Comparison of galaxy properties with and without spectroscopic information—redshifts (top left), stellar masses (top right), and dust attenuation values (bottom left) are shown. Marker shape indicates the field, color indicates the stellar mass estimated from photometry alone, and a filled symbol represents objects with ∣z phot − z spec∣ > 0.5. A clear discrepancy is seen between the UMG candidates (studied in previous works; purple points), which have generally good agreement, and the S-UMG candidates (the focus of this paper; yellow markers), which typically have different redshifts, lower stellar masses, and greater dust attenuation than predicted from photometry. Spectra exhibiting broad lines from AGN activity are marked with a cross. The bottom right panel shows the spectroscopically derived rest-frame colors for comparison with Figure 1. The redshift interlopers have extremely red rest-frame colors.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Comparison of UMGs selected from different photometric catalogs. Left side: the photometric redshifts and stellar masses of UMGs. The selection is represented by a black dashed box for comparison. In each row, either the UltraVISTA DR1 (top), COSMOS2020 CLASSIC EAzY-py (middle), or COSMOS2020 FARMER EAzY-py (bottom) catalog is used to select UMGs. The properties of the best matches to these objects in the other catalogs are shown in the other panels in that row. Objects with z phot < 1 are ostensibly due to photometric confusion between the Lyman- and Balmer-break features. Note that not all sources have a match in all catalogs. Right side: the location of UMGs on the rest-frame UVJ color–color diagram following the same scheme as the left side.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: S-UMG candidates with confirmed spectroscopic redshifts, in order of increasing z spec. Left: K-band imaging cutouts of the target, 7.″5 on a side. Center: the observed photometry of the galaxy (open circles) with best-fit models to the photometry alone (gray line) and photometric and spectroscopic data (gold line with cyan emission lines). Right: the observed spectrum binned in ∼19.5 Å bins (12 pixels in H band, 9 pixels in K band) is shown in black, with uncertainties in gray. Completely gray regions were not observed. The emission line model is again cyan added to the best-fit continuum model in orange. Note that the vertical ranges in the center and right panels are not the same.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: The K-band magnitudes (left), stellar masses derived from photometry (center), and UVJ rest-frame colors derived from photometry (right) of the MAGAZ3NE UMGs (11.0 < ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ < 11.7, purple) and S-UMGs (﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11.7, orange) candidates. The shape of a symbol indicates the field, either VIDEO-XMM (square), VIDEO-CDFS (circle), or COSMOS-UltraVISTA (star).
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Same as Figure 4 but for objects without confirmed spectroscopic redshifts. Best-fit models to the combined photometry and spectroscopy are shown in red.
Paper: Detection of Diffuse Hot Gas around the Young, Potential Superstar Cluster H72.97–69.39
Authors: Trinity L. Webb, Jennifer A. Rodriguez, Laura A. Lopez, Anna L. Rosen, Lachlan Lancaster, Omnarayani Nayak, Anna F. McLeod, Paarmita Pandey, Grace M. Olivier
Figure caption: Extracted, background-subtracted spectra from a 1﹩{}^{{\prime} }﹩ × 1﹩{}^{{\prime} }﹩ region around H72.97–69.39 with the best-fit thermal plasma model (a) and power-law model (b) overplotted. The best-fit parameters are listed in Table 2. Both models produce statistically good fits and predict similar X-ray luminosities from the source.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: The number density of massive galaxy candidates in the COSMOS field. Left: literature values for galaxies with ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11 from A. Muzzin et al. (2013a), Z. C. Marsan et al. (2022), and J. R. Weaver et al. (2022) are shown as gray, purple, and gold squares, respectively. Values from the FLAMINGO, GAEA, and TNG300 simulations convolved with a mass uncertainty of 0.25 dex are shown as orange, green, and blue lines, respectively, which truncate when the number of galaxies above the mass threshold drops below 10. The filled red star is the average number density from the seven COSMOS catalogs and SED modeling characterizations considered in Section 4, while the unfilled red star on the left panel shows the correction to this number density for galaxies with ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11.0 based on the MAGAZ3NE spectroscopic success rate, a correction of ∼10%. Right: literature values for galaxies with ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11.7 from A. Muzzin et al. (2013a), M. Stefanon et al. (2015), and J. R. Weaver et al. (2022) are shown as gray, black, and gold squares, respectively. The unfilled red arrows show the spectroscopic correction for galaxies with ﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11.7, which suggest a decrease of at least 4× (99% confidence) and possibly more than 17× (68% confidence).
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: The effects of different simulation comparison uncertainties. Left panels show UMGs and right panels show S-UMGs. FLAMINGO, GAEA, and TNG300 are shown in orange, green, and blue, respectively. Top row: the intrinsic number densities from simulations (dashed lines) compared to the values after resampling each stellar mass using a Gaussian of width 0.25 dex (solid lines). Second row: the scale of Poissonian uncertainties in each simulation (shaded areas). Values are truncated when the number of objects in the simulation passing the mass cut drops below 10. Third row: number densities resulting from different aperture selection. The FLAMINGO comparison includes lines for three projected aperture radii in physical units, as well as a spherical aperture with radius R 500c , where the density is 500 times the critical density of the Universe. The TNG300 comparison includes lines considering the total stellar mass in a subhalo, all stellar mass within the stellar half-mass radius, and all stellar mass within twice the stellar half-mass radius. Bottom row: number densities in the entire GAEA (500 h –1 Mpc)3 box (solid line), and those from (125 h –1 Mpc)3 subboxes. The median is shown as a dotted line, with shading between the 16th and 84th percentile values. Values are shown even when the number of galaxies in a bin are fewer than 10.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Line complex fitting for obtaining spectroscopic redshifts of candidate S-UMGs in the VIDEO-CDFS field with the same layout as Figure 2. For objects with confirmed redshifts, the region of the 1D and 2D spectrum with the confirming lines and fitted model are shown. The overall model is shown in red, while individual line components are shown in different colors (Hβ in blue, [O III] λλ4959, 5007 in green, Hα in orange, [N II] λλ6548, 6584 in purple, and [S II] λλ6718, 6733 in magenta). For objects without confirmed redshifts, the entire wavelength range probed by H- and K-band spectroscopy is shown. Some targets were observed with multiple masks which were sensitive to different wavelengths; in such cases regions covered by fewer than the total number of masks are displayed as a lighter shade of gray.
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: The same as Figure 6 but for the S-UMG sample selection (﹩{\rm{log}}({M}_{\ast }/{M}_{\odot })﹩ > 11.7).
Paper: MAGAZ3NE: Massive, Extremely Dusty Galaxies at z ∼ 2 Lead to Photometric Overestimation of Number Densities of the Most Massive Galaxies at 3 < z < 4 
Authors: Ben Forrest, M. C. Cooper, Adam Muzzin, Gillian Wilson, Danilo Marchesini, Ian McConachie, Percy Gomez, Marianna Annunziatella, Z. Cemile Marsan, Joey Braspenning, Wenjun Chang, Gabriella de Lucia, Fabio Fontanot, Michaela Hirschmann, Dylan Nelson, Annalisa Pillepich, Joop Schaye, Stephanie M. Urbano Stawinski, Mauro Stefanon, Lizhi Xie
Figure caption: Line complex fitting for obtaining spectroscopic redshifts of candidate S-UMGs in the VIDEO-XMM field. Same layout as Figure 2.