Seeing-Sorted Large Binocular Camera U-band Imaging of the Extended Groth Strip

Redshaw, Caleb; McCabe, Tyler; Otteson, Lillian; Windhorst, Rogier A.; Jansen, Rolf A.; Cohen, Seth H.; Carleton, Timothy; Ashcraft, Teresa; Nonino, M.; Paris, D.; Grazian, A.; Fontana, A.; Giallongo, E.; Speziali, R.; Testa, V.; Boutsia, K.; Koekemoer, Anton M.; O’Connell, R. W.; Rutkowski, Michael J.; Ryan, Russell E.; Scarlata, Claudia; Teplitz, Harry I.; Rafelski, Marc; Grogin, Norman A.

doi:10.3847/2515-5172/ac6189

Cited by 3 publications

(9 citation statements)

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“…Using the capabilities of the LBT/LBC for deep r-band imaging allows the detection of faint flux in galaxy outskirts in the form of star-forming clumps, tidal tails/mergers, and diffuse light. This paper builds upon the previous U-band work of Ashcraft et al (2018), Otteson et al (2021), Redshaw et al (2022) and T. McCabe et al (2023,in preparation) by utilizing the seeing sorted stacking procedure to create optimal depth and optimal resolution mosaics of GOODS-N for the r-band obtained simultaneously. Using these mosaics, we attempt to address the level to which faint, extended light in the outer regions of galaxies can contribute to the total observed EBL.…”

Section: Introductionmentioning

confidence: 87%

“…For each of the 838 individual exposures, the Gaussian FWHM was measured for unsaturated stars in the FOV, with the median value corresponding to the seeing of the entire exposure. As described in Ashcraft et al (2018), Otteson et al (2021) and Redshaw et al (2022), this allows for a seeing distribution to be created for the entire data set as shown in Figure 1. The median FWHM for all images is ∼1 07, which is marginally larger than the typical seeing conditions on Mt.…”

Section: Creating R-band Mosaicsmentioning

confidence: 99%

“…Prior to creating the mosaics, the relative transparency was calculated for each of the 838 exposures following the prescription in Otteson et al (2021), Redshaw et al (2022) and McCabe et al (2022;in preparation). In order to account for the night to night differences in relative atmospheric transparency, the flux ratio between ∼100 unsaturated stars was taken with respect to the flux values from the Sloan Digital Sky Survey (SDSS) Data Release 16 (Blanton et al 2017;Ahumada et al 2020) in the r-band.…”

Section: Creating R-band Mosaicsmentioning

confidence: 99%

“…The Large Binocular Telescope (LBT) is able to obtain imaging for 4 of the 5 CANDELS (Grogin et al 2011;Koekemoer et al 2011) fields that are in the northern hemisphere or around the celestial equator (Ashcraft et al 2018;Otteson et al 2021;Redshaw et al 2022, T. McCabe et al 2023. Ashcraft et al (2018) presented ultra deep U-band imaging of GOODS-N (Giavalisco et al 2004) and created optimal resolution and optimal depth mosaics, which represent the best U-band imaging that can be achieved from the ground.…”

Section: Introductionmentioning

confidence: 99%

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Deep Large Binocular Camera r-band Observations of the GOODS-N Field

Ashcraft

McCabe

Redshaw

et al. 2023

PASP

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We obtained 838 Sloan r-band images (∼28 hr) of the GOODS-North field with the Large Binocular Camera (LBC) on the Large Binocular Telescope in order to study the presence of extended, low surface brightness features in galaxies and investigate the trade-off between image depth and resolution. The individual images were sorted by effective seeing, which allowed for optimal resolution and optimal depth mosaics to be created with all images with seeing FWHM < 0.″9 and FWHM < 2.″0, respectively. Examining bright galaxies and their substructure as well as accurately deblending overlapping objects requires the optimal resolution mosaic, while detecting the faintest objects possible (to a limiting magnitude of m AB ∼ 29.2 mag) requires the optimal depth mosaic. The better surface brightness sensitivity resulting from the larger LBC pixels, compared to those of extant WFC3/UVIS and ACS/WFC cameras aboard the Hubble Space Telescope allows for unambiguous detection of both diffuse flux and very faint tidal tails. Azimuthally-averaged radial surface brightness profiles were created for the 360 brightest galaxies in each of the two mosaics. On average, these profiles showed minimal difference between the optimal resolution and optimal depth surface brightness profiles. However, ≲15% of the profiles show excess flux in the galaxy outskirts down to surface brightness levels of μ r AB ≃ 31 mag arcsec−2. This is relevant to Extragalactic Background Light (EBL) studies as diffuse light in the outer regions of galaxies are thought to be a major contribution to the EBL. While some additional diffuse light exists in the optimal depth profiles compared to the shallower, optimal resolution profiles, we find that diffuse light in galaxy outskirts is a minor contribution to the EBL overall in the r-band.

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Section: Introductionmentioning

confidence: 87%

Section: Creating R-band Mosaicsmentioning

confidence: 99%

Section: Creating R-band Mosaicsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Deep Large Binocular Camera r-band Observations of the GOODS-N Field

Ashcraft

McCabe

Redshaw

et al. 2023

PASP

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“…As part of the GOODS-N UVCANDELS observations, Ashcraft et al (2018) used the capabilities of the Large Binocular Camera (LBC) on the Large Binocular Telescope (LBT) to complement the Hubble Space Telescope (HST) parallel WFC3/UVIS F275W and ACS/WFC F435W observations with ground based U-band (λ c ; 359 nm; Δλ ; 54 nm) imaging. Ashcraft et al (2018) pioneered the seeing sorted stacking method, which was used by Otteson et al (2021); Redshaw et al (2022) and Ashcraft et al (2023) to stack individual exposures (starting with the best seeing) incrementally to create "optimal depth" and "optimal resolution" mosaics. The optimal resolution and optimal depth stack FWHM cutoffs were dependent upon the seeing distributions for each individual exposure, but only the best ∼10% of the exposures were used for the optimal resolution mosaic and only the worst ∼5%-10% were excluded from the optimal depth mosaic.…”

Section: Introductionmentioning

confidence: 99%

Searching for Intragroup Light in Deep U-band Imaging of the COSMOS Field

McCabe

Redshaw

Otteson

et al. 2023

PASP

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We present the results of deep, ground based U-band imaging with the Large Binocular Telescope of the Cosmic Evolution Survey field as part of the near-UV imaging program, UVCANDELS. We utilize a seeing sorted stacking method along with night-to-night relative transparency corrections to create optimal depth and optimal resolution mosaics in the U-band, which are capable of reaching point source magnitudes of AB∼26.5 mag at 3σ. These ground-based mosaics bridge the wavelength gap between the Hubble Space Telescope WFC3 F275W and ACS F435W images and are necessary to understand galaxy assembly in the last 9–10 Gyr. We use the depth of these mosaics to search for the presence of U-band intragroup light (IGrL) beyond the local universe. Regardless of how groups are scaled and stacked, we do not detect any U-band IGrL to unprecedented U-band depths of ∼29.1–29.6 mag arcsec−2, which corresponds to an IGrL fraction of ≲1% of the total group light. This stringent upper limit suggests that IGrL does not contribute significantly to the Extragalactic Background Light at short wavelengths. Furthermore, the lack of UV IGrL observed in these stacks suggests that the atomic gas observed in the intragroup medium is likely not dense enough to trigger star formation on large scales. Future studies may detect IGrL by creating similar stacks at longer wavelengths or by pre-selecting groups which are older and/or more dynamically evolved similar to past IGrL observations of compact groups and loose groups with signs of gravitational interactions.

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Lyman Continuum Emission from Active Galactic Nuclei at 2.3 ≲ z ≲ 3.7 in the UVCANDELS Fields

Smith,

Windhorst,

Teplitz

et al. 2024

ApJ

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We present the results of our search for Lyman continuum (LyC)-emitting (weak) active galactic nuclei (AGN) at redshifts 2.3 ≲ z ≲ 4.9 from Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) F275W observations in the Ultraviolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (UVCANDELS) fields. We also include LyC emission from AGN using HST WFC3 F225W, F275W, and F336W imaging found in Early Release Science (ERS) and Hubble Deep UV Legacy Survey data. We performed exhaustive queries of the Vizier database to locate AGN with high-quality spectroscopic redshifts. In total, we found 51 AGN that met our criteria within the UVCANDELS and ERS footprints. Out of these 51, we find 12 AGN that had ≥4σ detected LyC flux in the WFC3/UVIS images. Using a wide variety of space-based plus ground-based data, ranging from X-ray to radio wavelengths, we fit the multiwavelength photometric data of each AGN to a CIGALE spectral energy distribution (SED) using AGN models and correlate various SED parameters to the LyC flux. Kolmogorov–Smirnov tests of the SED parameter distributions for the LyC-detected and nondetected AGN showed they are likely not distinct samples. However, we find that the X-ray luminosity, star formation onset age, and disk luminosity show strong correlations relative to their emitted LyC flux. We also find strong correlations of the LyC flux to several dust parameters, i.e., polar and toroidal dust emission and 6 μm luminosity, and anticorrelations with metallicity and A FUV. We simulate the LyC escape fraction (f esc) using the CIGALE and intergalactic medium transmission models for the LyC-detected AGN and find an average f esc ≃ 18%, weighted by uncertainties. We stack the LyC fluxes of subsamples of AGN according to the wavelength continuum region in which they are detected and find no significant distinctions in their LyC emission, although our submillimeter-detected F336W sample (3.15 < z < 3.71) shows the brightest stacked LyC flux. These findings indicate that LyC production and escape in AGN are more complicated than the simple assumption of thermal emission and a 100% escape fraction. Further testing of AGN models with larger samples than presented here is needed.

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Seeing-Sorted Large Binocular Camera U-band Imaging of the Extended Groth Strip

Cited by 3 publications

References 12 publications

Deep Large Binocular Camera r-band Observations of the GOODS-N Field

Deep Large Binocular Camera r-band Observations of the GOODS-N Field

Searching for Intragroup Light in Deep U-band Imaging of the COSMOS Field

Lyman Continuum Emission from Active Galactic Nuclei at 2.3 ≲ z ≲ 3.7 in the UVCANDELS Fields

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