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

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

doi:10.1088/1538-3873/aca1e0

Cited by 3 publications

(6 citation statements)

References 67 publications

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“…Observations of a wider range of group environments could provide insight into the build up of IGrL through galaxy interactions and/or tidal stripping. In Ashcraft et al (2023), evidence of additional diffuse light in the outskirts of galaxies was detected in the r-band resulting from tidal tails and galaxy interactions. These signs of interactions have also been abundantly observed with JWST (Finkelstein et al 2022;Windhorst et al 2023, and references therein).…”

Section: Discussion and Summarymentioning

confidence: 99%

“…We used 25 partial nights with the LBT/LBC between 2007 and 2020 to observe the COSMOS field in the Uband and create optimal resolution and optimal depth mosaics totaling up to ∼37 hr. Following the seeing sorted stacking process detailed in Ashcraft et al (2018), Otteson et al (2021), Redshaw et al (2022) and Ashcraft et al (2023), the seeing of each individual exposure was calculated through the median FWHM of ∼100 unsaturated stars. Prior to creating the optimal resolution (FWHM 0 9) and optimal depth (FWHM 1 9) mosaics, the relative atmospheric transparency was corrected for each exposure.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…Graham (Taylor et al 2004;Ashcraft et al 2018). In order to address this slight offset, we investigated the relative transparency of each of the following the procedures described in Otteson et al (2021), Redshaw et al (2022) and Ashcraft et al (2023). For each individual exposure, a subset of ∼150 unsaturated stars was selected from a Sloan Digital Sky Survey (SDSS) Data Release 16 (Blanton et al 2017;Ahumada et al 2020) based catalog of stars with U-band magnitudes, 18 u 22 mag.…”

Section: Floating Zero Point Correctionmentioning

confidence: 99%

“…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%

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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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Section: Discussion and Summarymentioning

confidence: 99%

Section: Discussion and Summarymentioning

confidence: 99%

Section: Floating Zero Point Correctionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

McCabe

Redshaw

Otteson

et al. 2023

PASP

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“…To create the full-field mosaics, we followed a procedure similar to those of Ashcraft et al (2018Ashcraft et al ( , 2023 and McCabe et al (2023), where images in a given filter are combined in two different ways: one to optimize the spatial resolution at the cost of depth, and the other to optimize the depth at the cost of resolution. In those works, the optimal resolution images result from stacking the best-seeing images, comprising about 10% of the total number of images (Ashcraft et al 2018), while for the optimal depth, the 5%-10% worst-seeing images are excluded (Ashcraft et al 2018;McCabe et al 2023); typically, the cutoff is made at ∼2 0, with the deeper mosaic reaching ∼1 mag fainter than the higher-resolution mosaic (McCabe et al 2023).…”

Section: Mosaicsmentioning

confidence: 99%

PEARLS: Near-infrared Photometry in the JWST North Ecliptic Pole Time Domain Field*

Willmer,

Ly,

Kikuta

et al. 2023

ApJS

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We present near-infrared (NIR) ground-based Y, J, H, and K imaging obtained in the James Webb Space Telescope (JWST) North Ecliptic Pole Time Domain Field (NEP TDF) using the MMT-Magellan Infrared Imager and Spectrometer on the MMT. These new observations cover a field of approximately 230 arcmin2 in Y, H, and K, and 313 arcmin2 in J. Using Monte Carlo simulations, we estimate a 1σ depth relative to the background sky of (Y, J, H, K) = (23.80, 23.53, 23.13, 23.28) in AB magnitudes for point sources at a 95% completeness level. These observations are part of the ground-based effort to characterize this region of the sky, supplementing space-based data obtained with Chandra, NuSTAR, XMM, AstroSat, Hubble Space Telescope, and JWST. This paper describes the observations and reduction of the NIR imaging and combines these NIR data with archival imaging in the visible, obtained with the Subaru Hyper-Suprime-Cam, to produce a merged catalog of 57,501 sources. The new observations reported here, plus the corresponding multiwavelength catalog, will provide a baseline for time-domain studies of bright sources in the NEP TDF.

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

Cited by 3 publications

References 67 publications

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

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

PEARLS: Near-infrared Photometry in the JWST North Ecliptic Pole Time Domain Field*

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

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