adsabs/AstroCLIMB huggingface dataset:
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: The recovery completeness of injected transit signals into the light curve of TOI 4633 as a function of the radius and orbital period. The radius of planet candidate b was estimated using the planet mass–radius scaling relations for volatile-rich planets by Otegi et al. (2020). The signals were recovered using a BLS search. The figure clearly highlights that if planet candidate b were aligned such that it would transit star A, the transit events would have been detected by the BLS search algorithm.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: 100 orbits randomly drawn from the posterior distribution of the ORBITIZE! model (gray lines) for the angular separations (top panel) and position angle (bottom panel) of TOI 4633 AB. The best-fit models constructed from the median of the posteriors of each parameter are shown in black, and the residuals to these models are shown below each panel. Archival astrometric data, which have no uncertainties reported in the literature, are shown by the black points. We adopted large uncertainties for these archival position angles and angular separations of ± 10 deg and ± 50 mas, respectively. All newly obtained data with reported uncertainties are shown in orange.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Binary semimajor axis vs. planet period for planetary systems with more than one star. Transiting planets are shown as triangles, while radial velocity-detected planets are shown as crosses. TOI 4633 planets are shown in red. TOI 4633 has a smaller binary separation than most planet-hosting binary systems, and TOI 4633 c is the longest-period transiting planet currently known in a binary system.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: RV time-series (top) and phase-folded plots for TOI 4633 b (lower left) and TOI 4633 c (lower right). SOPHIE (blue circles) and HIRES (orange diamonds) RV measurements are shown following the subtraction of the systemic velocities for each instrument. The light colored error bars show the uncertainties accounting for the jitter. Solid black lines show the inferred median model. Gray lines show models made with 100 random samples from the posterior distributions.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Phase-folded light curve for TOI 4633 c. 2 minutes and 20 s cadence TESS observations are shown in light gray. Solid color circles represent 60 minutes binned data. The inferred transit model is shown with a solid black line.
Paper: The Digitization of Photographic Spectra in the Dominion Astrophysical Observatory Plate Collection with Commercial Scanners: A Pilot Study
Authors: T. J. Davidge
Figure caption: Scanned spectra of Vega recorded on 1925 August 14 and 1949 October 28 with the 1.8 m telescope and the Cassegrain spectrograph. The front of the protective envelope for each plate is also shown. The plates are 10 × 5 cm in size. These plates show the range of calibration information that might be expected in the 1.8 m plate collection. The stellar spectrum, emission arcs, and linearity calibration information are indicated. Arcs were not recorded with the 1949 spectra. The linearity calibration information is restricted to a series of dots to the right of the 1925 Vega spectrum. In contrast, there is a staircase-like linearity assessment region that parallels the dispersion axis of the 1949 spectra. This calibration area is saturated in some locations and is subject to smearing from scattered light.
Paper: The Digitization of Photographic Spectra in the Dominion Astrophysical Observatory Plate Collection with Commercial Scanners: A Pilot Study
Authors: T. J. Davidge
Figure caption: Background light subtraction in the 1963 plate. The panels show a cross section perpendicular to the dispersion direction before and after background subtraction. This cut samples a wavelength near Hγ. Light from the stars, arcs, and linearity calibration region swamp the background light in the central regions of the cut. The green lines mark the approximate regions used to fit the large-scale linear trend in background light that was subtracted from the data. While much of the variation in the background regions is suppressed with the removal of a linear trend, the upward-pointing signal in the left-hand edge of the background-subtracted panel indicates that a linear fit to the background is only an approximation.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: We find that the extent to which planet signals can be isolated from the observed spectra is driven by two factors: the planet pixel shift, N px, and the ratio of out-of-transit spectra to in-transit spectra, N out/N in. Left: the S/N across the space spanned by these two parameters is shown, for the case of recovering a CH4 model injected with N in  = 16, using five PCA iterations. The S/N given is the median found when sampling injections over a large number of possible V sys. Increasing ability to detrend, represented by an increase in recovered S/N, is demonstrated when increasing either N px or N out/N in. With few out-of-transit spectra, it is very difficult to recover low-velocity (N px ≲ 3) signals. The N px value for the planet, TOI-732 c, and instrument in this study without the barycentric contribution is marked in white (N px = 1.3; see Table 2). In the case shown here, a significant signal can be recovered for this planet and model when the number of out-of-transit spectra ≳0.8× the number of in-transit spectra. Right: for the case of N px  = 1.5, similar to that of TOI-732 c, the median S/N across V sys is shown against the out-of-transit to in-transit ratio. A significant increase in S/N is found as more out-of-transit spectra are observed.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: S/N maps for high-velocity injection and recovery tests, for comparison to those for the low-velocity injection tests shown in Figure 2. The injected K p and V sys  are the same as for the low-radial-velocity-change case, with the transit duration of the injected signal multiplied to simulate the larger planet pixel shift of N px  = 25, in accordance with Figure 8, and consistent with the high-velocity case used in Figures 1 and 10. The number of principal components subtracted during detrending is six, nine, and seven for each of NH3, CH4, and H2O, respectively. S/N values of 7.5, 5.7, and 4.3 are obtained for NH3, CH4, and H2O, respectively, with the recovered K p constrained in each case. It should be noted that the noise remaining in the data is greater for the high-velocity case than the low-velocity case, and therefore the recovered S/N is not proportional to the fraction of signal remaining, as given in Figure 1.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: The low-velocity H2O planet signal, initially seen using cross-correlation (see the right-hand panel of Figure 2), is now recovered using a Bayesian log-likelihood approach. As before, the planet model was injected into the data with K p = 70 km s−1 and V sys  = 20 km s−1, for 21 in-transit and 12 out-of-transit spectra. Top: by comparing the detrended spectral residuals with a reprocessed model, and marginalizing over α, a detection significance is calculated across K p−V sys space. Bottom: the posterior probability distribution across V sys−α space is shown, with values of V sys  = 20 ± 2 km s−1 and α = 0.8 ± 0.2 found. In both cases, a signal is recovered with parameters consistent with the injection (marked with a red cross/crosshairs). A final detection significance of 2.9σ is achieved for H2O compared with the null model. Note that this is smaller than the peak significance shown in the top panel, where only α has been marginalized, since we are no longer assuming perfectly known K p and V sys at each point.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: The extent to which a planet signal can be recovered increases with the planet pixel shift, N px, or number of pixels across which the planetary signal is spread. The detection S/N of a CH4 signal, injected with a V sys of −15 km s−1 into 16 in-transit spectra, with 12 out-of-transit spectra, and detrended by subtracting three principal components, is shown as a function of K p−﹩{\phi }_{\max }﹩ space. Contours showing lines of constant N px, calculated using the resolution of the IGRINS data used here, are shown, aligning strongly with the increase in S/N. This trend begins to slow at higher values of N px. Signals with changes in radial velocity less than that corresponding to one instrument resolution element can still be recovered. The barycentric velocity correction is here set to zero, and due to the even number of in-transit spectra simulated, ﹩{\phi }_{\max }﹩ here represents half the in-transit phase range of each simulation.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: The degradation of the planet signal by PCA varies for different numbers of out-of-transit observations. Similar to Figure 1, an NH3 signal is used here, with the rate of signal removed with each principal component subtracted explored across N out/N in space. With no out-of-transit spectra, the signal is effectively entirely removed after one iteration of PCA, consistent with Figure 5. Observing more out-of-transit spectra slows this removal, giving the trend in S/N seen in Figure  9. A higher-velocity signal is also shown for comparison.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: Low-velocity planet signals can still be recovered from partial transits although to a lower significance. In each case shown here the signal has been injected into 21 in-transit spectra with a planetary velocity of K p = 70 km s−1. There are 12 out-of-transit spectra in both plots, but whereas in Figure 2 these are split equally between pre- and posttransit, here they are all either before or after the transit. Top: for 12 pretransit spectra, the signal is recovered with a S/N of 3.1. Bottom: for 12 posttransit spectra, the signal is recovered with a S/N of 3.9.
Paper: Feasibility of High-resolution Transmission Spectroscopy for Low-velocity Exoplanets
Authors: Connor J. Cheverall, Nikku Madhusudhan
Figure caption: S/N maps obtained for each of NH3, CH4, and H2O, when using the raw spectra rather than first dividing by the spectrum of an A0V telluric standard star, as was done throughout the rest of this work. The signals continue to be recovered, with S/N values consistent with before (5.0 for NH3, 3.4 for CH4, and 1.6 for H2O).
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: FUV image of WLM showing the field of view from ALMA Cycle 1 (smaller cyan squares; Rubio et al. 2015) and Cycle 6 (larger cyan rectangle; M. Rubio et al. 2024, in preparation) and the 45 detected CO cores (tiny orange circles), along with the field of view from JWST ERS PID 1334 (green squares; Weisz et al. 2023). The ERS fields will be referred to as the North field and the South field. The orientation of the image is such that North is up and East is to the left. Color-bar values can be converted from counts/second to calibrated AB magnitudes with the equation: FUV A B  = −2.5log10 (FUV ﹩{}_{\mathrm{counts}\,{\rm{s}}}^{-1})+18.82﹩.
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Left panel: Faraday depth of the dominant RM synthesis component for the MeerKAT calibrators compared to the RM from the NVSS (black circles) and dominant Faraday depth component from SPASS (green squares). Right panel: the percent polarization from MeerKAT compared to NVSS (black) and SPASS (green).
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: RM synthesis amplitude spectra for the ten sources in Table 2. The spectra are dominated by a single RM component close to zero. The high sidelobes are caused by the missing frequency ranges (see, for example, Figure 3.)
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Distribution of linear fractional polarization p med for the calibrator sources.
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Fractional polarization spectral index vs. total intensity spectral index for 69 sources detected in polarization.
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Fractional band-averaged circular polarization (%) vs. the MeerKAT spectral index from the Stokes I spectrum. Sources with measured values of v med > 0.07% are shown in red.
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Distribution of band-averaged fractional Stokes V (%) for the MeerKAT calibrator sources.
Paper: A MeerKAT Polarization Survey of Southern Calibration Sources
Authors: A. R. Taylor, L. S. Legodi
Figure caption: Comparison of the flux density at 1400 MHz from MeerKAT and NVSS. The dashed line shows the 1:1 relation.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Top: F090W vs. F090W–F150W CMD for all objects (red: in FUV knots and near CO; blue: in FUV knots and away from CO; and yellow: away from FUV knots and away from CO). The blackbody temperature corresponding to the F090W–F150W color is shown on the top x-axis, and the reddening vector A  V  = 1 assuming SMC-like extinction is included in the upper right of the plot. Bottom: F250M vs. F250M–F430M CMD for all objects. The blackbody temperature corresponding to the F250M–F430M color is shown on the top x-axis and the temperature range from the F090W vs. F090W–F150W CMD is shaded in gray. The reddening vector A  V  = 20 assuming SMC-like extinction is included in the upper right of the plot.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: FUV image of JWST ERS south field overlaid with type 1 objects (in FUV and near CO, red circles), type 2 objects (in FUV and away from CO; blue circles), type 3 objects (away from FUV and away from CO; yellow), resolved background galaxies (magenta circles), and CO cores (orange circles). The orientation of the image is such that north is up and east is to the left. Color-bar values can be converted from counts/second to calibrated AB magnitudes with the equation: FUV A B  = −2.5log10 (FUV﹩{}_{\mathrm{counts}\,{\rm{s}}}^{-1})+18.82﹩.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: FUV image of JWST ERS north field overlaid with type 1 objects (in FUV and near CO, red circles), type 2 objects (in FUV and away from CO; blue circles), type 3 objects (away from FUV and away from CO; yellow), resolved background galaxies (magenta circles), and CO cores (orange circles). The orientation of the image is such that north is up and east is to the left. Color-bar values can be converted from counts/second to calibrated AB magnitudes with the equation: FUV A B  = −2.5log10 (FUV﹩{}_{\mathrm{counts}\,{\rm{s}}}^{-1})+18.82﹩.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Color–color diagram of F090W–F150W vs. F250M–F430M for all objects (red circles: in FUV knots and near CO; blue circles: in FUV knots and away from CO; and yellow circles: away from FUV knots and away from CO) including seven resolved background galaxies (light purple stars). A reddening vector of A  V  = 1 assuming SMC-like extinction is included in the upper left of the plot, and the black line shows the effective temperature of a blackbody.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Comparison of object masses computed using PROSPECTOR vs. the TIR luminosity for all three object types, where the TIR luminsoity method assumes an age of 1 Myr (top) or an age of 10 Myr (bottom). The gray line shows where the masses computed using both methods are the same.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of JWST ERS south field overlaid with type 1 objects (in FUV and near CO; red circles), type 2 objects (in FUV and away from CO; blue circles), type 3 objects (away from FUV and away from CO; yellow), resolved background galaxies (magenta circles), and CO cores (orange circles). The orientation of the image is such that north is up and east is to the left.