ner_tags: O O O O O O O O O O B-Instrument O O O O O B-Telescope O O O O O O O O O O B-Wavelength B-Model O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O B-Telescope O O O O O O O B-CelestialObject O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O B-Instrument O O O O O O B-Telescope B-Instrument O O O O O O O O O O O O O O O O O B-Instrument O O B-CelestialObject O B-Instrument O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O B-Telescope B-Instrument O O O O O O O O O B-Telescope O B-Telescope O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O O O O O O B-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software O O B-Software O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O B-Software I-Software I-Software B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O B-Software O O O O O O O B-Model I-Model I-Model I-Model O O O O O O O B-Software O O O O O O O O O
tokens: of all neighboring sources in 120 radius fitting to the IRAC frame a higher-resolution image (the HST detection mosaic) convolved with a kernel reconstructed from the empirical IRAC PSFs and the PSF of the prior image. Aperture photometry (with a diameter of 18) is then performed after removing the models of the neighboring objects. A correction based on the PSF and on the light profile of the source under analysis is finally applied to obtain total fluxes. Table 4 gives the observed IRAC fluxes. As with the HST data, the photometry has been corrected for Galactic extinction (Schlafly Finkbeiner 2011 ), although this extinction does not affect the measurements, given the lack of precision in the IRAC data. Table 4 Candidate Super Eight Spitzer IRAC Magnitudes Notes. The 1 σ uncertainties are quoted for the non-detection upper limits. a There are no IRAC observations for Super8-6. The IRAC uncertainties were measured in the same manner as described in Stefanon et al. ( 2017 ). Briefly, the rms was calculated for the pixels in the apertures using the residual frames (science frame with all objects subtracted). Systematic errors from the kernel reconstruction are also taken into account and the final result was scaled using the aperture correction. We present the cutouts from the available HST bands in Figure 1 – 8 , as well as the Spitzer IRAC cutouts for the objects with available data. Figure 1. HST and Spitzer cutouts for Super8-1. The cutouts are 5′′ × 5′′ and centered on the candidate galaxy. The central circles have a radius of 09, matching the IRAC aperture, and are included to guide the eye. For the IRAC cutouts, both the original images (top) and images after neighbor subtraction (bottom) are shown. The bottom right figure gives the photometry and fit SED for Super8-1. The observed photometry is shown with black open squares, while the fit is shown with dark pink open circles. The fit spectrum is shown with a solid pink line. The upper limits indicate the 1 σ uncertainties. The probability distributions from the redshift fitting performed using EAZY (pink) and BPZ (green) are given in the lower rightmost panel. Figure 2. Same as Figure 1 but for Super8-2. Figure 3. Same as Figure 1 but for Super8-3. Figure 4. Same as Figure 1 but for Super8-4. Figure 5. Same as Figure 1 but for Super8-5. Figure 6. Same as Figure 1 but for Super8-6. Figure 7. Same as Figure 1 but for Super8-7. Figure 8. Same as Figure 1 but for Super8-8. 4. Photometric Redshift Fitting We performed photometric redshift fitting using the EAZY fitting code (Brammer et al. 2008 ). This algorithm can quickly fit linear combinations of spectral templates that are based on semianalytic models (SAMs), rather than spectroscopic samples. Brinchmann et al. ( 2017 ) determined that the least-biased EAZY template for high-redshift galaxy fitting is the eazy _ v1.3 template. This template is based on the original EAZY template that was developed from synthetic galaxy photometry using