adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Size of the 1.4 μm feature against planet temperature and subdivided by the planet’s surface gravity. At lower temperatures, the surface gravity may have an impact on the cloudiness of the planet, and thus the feature size, but at higher temperatures there appears to be no obvious correlation. Gray regions highlight the expected feature size for solar-metallicity atmospheres for a given cloud pressure and a surface gravity between 10 and 20 m s−2. Across the entire population, the mean 1.4 μm feature size is 0.81 scale heights in the HST/WFC3/G141 while the median is 1.37. The feature size can be directly correlated to the retrieved cloud pressure from our retrievals (bottom), and we note that the 1.4 μm feature size is not a good predictor of the feature size across wider wavelength ranges due to the stronger absorption seen at longer wavelengths. The priors for the cloud pressure in our retrievals are shown by the dotted lines.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Ratio of H2O-to-H with respect to stellar metallicity values for the planets from our study. The recovered values from Welbanks et al. (2019) are also shown, as are their best-fit trends. Top: BHM results when only using retrievals which give a >3σ atmospheric detection. Bottom: BHM results when using retrievals which give a >2σ atmospheric detection. In the former case, the BHM found a best-fit trend line which had a negative slope while the latter had a positive slope. However, in both cases the null hypothesis (metallicity is not dependent upon mass) was preferred. Additionally, either sign of slope, or indeed no slope, is also within the 1σ errors of each fit.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Retrieved metallicity when a simulated data set is created using the model from Thorngren et al. (2016). From our fake data sets, which utilized the error bars from the real observations as well as the retrieved 10 bar radius and cloud pressure, we can recover the input trend, albeit a marginal detection due to the size of the uncertainties on the planet’s metallicity. The finding contrasts the real data, where no obvious trend was uncovered.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: White light curves for scanning-mode data of GJ1214 b on 2013 August 4 (top) and 12 (bottom). The residuals of the in-transit orbit are non-Gaussian, and this could be caused by starspot crossing.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Transit spectra of GJ1214 b using different amalgamations of data sets. All are roughly consistent with one another, and the spectrum used for atmospheric analyses in this study is shown in black.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the 1.4 μm feature height to different bulk parameters for the sub-Neptunes within our study. Red data points indicate those studied by Crossfield & Kreidberg (2017) with their trends also shown in red. Our trends are shown in black and are linear fits, except for with temperature, where a second-order polynomial fit was used.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the Bayesian evidence for retrievals with free chemistry and those using the GGChem chemical equilibrium scheme.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit spectrum of CoRoT-1b obtained here to those in the literature. While the features within the spectra are similar, there are offsets between different studies.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparisons of different spectra for HIP 41378 f. All spectra derived in this work exhibit features while the result from Alam et al. (2022) is flat. Two pipelines were used here to check the result. They give slightly different mean depths and the Cascade spectrum has a decreasing slope at shorter wavelengths. Utilizing the wavelength bins and limb-darkening coefficients from Alam et al. (2022) did not remedy the situation.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Left: comparison of the spectrum derived in this work of HD 97658 b to that from Knutson et al. (2014), who only analyzed visits 1 and 2. Other than a slight offset, the spectra agree well after two visits but the averaged spectrum of all four transits has a stronger slope. Right: comparison of the spectrum derived in this work of HD97658 b, to that from Guo et al. (2020). While the spectra agree over 1.3–1.5 μm, outside of this range there is a significant disagreement in the features.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Left: uncorrected transit spectra for each visit of TOI-270 c. The shaded regions indicate the white light-curve depth, and 1σ uncertainty, for each visit. Right: normalized transit spectra for each visit of TOI-270 c. The averaged transit spectrum, which was used in the analysis here, is given in black.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: White light-curve fits for the observations of V1298 Tau b (top) and V1298 Tau c (bottom). We note the non-Gaussian residuals in each case, potentially due to stellar activity.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit spectrum of TrES-4 b obtained here to the spectrum from Ranjan et al. (2014).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit spectrum of TrES-2 b obtained here to the spectrum from Ranjan et al. (2014).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit depths obtained here to those from Van Eylen et al. (2021) for TOI-270 c (left) and TOI-270 d (right). As previously noted, we find a large variance in the transit depth obtained for each visit of TOI-270 c and only one of these is of a similar depth to the TESS data.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Spectrum of HIP 41378 f recovered with Iraclis and the preferred models from our retrievals.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Retrieved abundances of TiO against planet equilibrium temperature. In some cases, only an upper bound on the presence of the molecule could be placed and, for these, the error bar extends to log10(VMR) = −12. The filled regions bounded by dashed gray lines indicate the predicted abundances from GGchem chemical equilibrium models (assuming C/O = 0.54 and solar metallicity) across 1 × 102 to 1 × 105 Pa (1 × 10–3 to 1 bar). Left: the thick colored line on each plot indicates the linear trend from the BHM while the thinner colored lines represent the traces from the fit that were within the 1σ errors of the best-fit model. Right: the same except for the flat model (i.e., the null hypothesis). Top: black data points indicate planets for which the retrieval model with optical absorbers is preferred, while gray points represent those for which a preferable fit is obtained without them. In these plots, all these retrieval traces were used in the BHM. Bottom: only the retrievals for which the optical absorber model was preferred.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Retrieved abundances of H2O, CH4, HCN, and NH3 against planet equilibrium temperature. In some cases, only an upper bound on the presence of the molecule could be placed and, for these, the error bar extends to log10(VMR) = −12. The filled regions bounded by dashed gray lines indicate the predicted abundances from GGchem chemical equilibrium models (assuming C/O = 0.54 and solar metallicity) across 1 × 102 to 1 × 105 Pa (1 × 10–3 to 1 bar). Left: the thick colored line on each plot indicates the linear trend from the BHM while the thinner colors lines represent the traces from the fit that were within the 1σ errors of the best-fit model. Right: the same except for the flat model (i.e., the null hypothesis).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Top: spectrum of V1298 Tau b recovered with Iraclis and the preferred models from our retrievals. Bottom: the probability distributions for the planetary mass when it was fitted for. We note that, while it gives a preferable fit to the data, the fitted mass is extremely low (a value of 0.64 M J was recovered by Suárez Mascareño et al. 2021). The optical absorber model is unlikely for this planet given the equilibrium temperature (∼1000 K).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit spectrum of WASP-107 b obtained here to the spectrum from Kreidberg et al. (2018a) and Spake et al. (2018).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Top: spectrum of V1298 Tau b recovered with Iraclis and the preferred models from our retrievals. Bottom: the probability distributions for the planetary mass when it was fitted for. The optical absorber model is preferred, but it is unlikely that FeH and e− are present in the atmosphere of this planet given the equilibrium temperature (∼700 K).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the retrieved metallicity when the C/O ratio is a free parameter to when it is fixed to 0.5 (top) and 1 (bottom). We only show planets with our sample which have a strong (>3σ) atmosphere detection.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the transit spectrum of WASP-6 b obtained here to the spectrum from Carter et al. (2020).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Same as Figure 33 but for VO.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the Bayesian evidence for the fixed C/O ratio retrievals when it is fixed to 0.5 (top) and 1 (bottom). The dotted line shows the 3σ region.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Comparison between IRAC [3.6] mag in this catalog and the aperture-based SHELA IRAC catalog (Papovich et al. 2016, P16) for sources with different models. The black dashed lines show the expected 1σ magnitude difference due to photometric uncertainties in both catalogs as a function of magnitude. The magnitudes in P16 are measured in Kron apertures. The unresolved PointSource model results in similar magnitudes, while the resolved SimpleGalaxy, DevGalaxy, and ExpGalaxy models result in brighter magnitudes in this catalog. The spread of magnitude for the PointSource and SimpleGalaxy models is within the expectations from photometric uncertainties, while the more resolved DevGalaxy and ExpGalaxy models produce brighter fluxes beyond the expected 1σ spread. This suggests that model-based photometry is more capable of capturing all of the flux from resolved sources.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Demonstration of our measurement of flux error by simulation of injected sources in the DECam r, NEWFIRM K  s , and IRAC [3.6] bands in T1. The data points and error bars show the median and central 68th percentiles of the fractional flux difference between the injected and recovered sources, respectively, in each magnitude bin. The shaded region shows the median fractional error reported by The Farmer (σ Farmer/F in). The dotted, dashed, and solid black lines show the best-fit systematic, statistical, and total errors, respectively, as defined in Equation (6). The recovered error is substantially larger than the error reported by The Farmer in the NEWFIRM and IRAC bands. This is likely due to a combination of larger PSF and native pixel sizes, resulting in more correlated pixels.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Differential number counts of galaxies vs. HSC riz and NEWFIRM K  s  magnitudes. The Poisson error bars are smaller than the data point markers. The dashed lines show the galaxy number counts in Koushan et al. (2021), and the black solid line shows the best-fit line in Gawiser et al. (2006). Our measured number counts agree with the reported relation up to our 50% completeness limit of r ≈ 25, beyond which the number counts fall below the relation. A slight excess of bright galaxies is observed at m ≲ 20. This difference could by caused by the increase in measured flux for bright, resolved galaxies in model-based photometry.