New Photometric Calibration of the Wide Field Camera 3 Detectors

Calamida, A.; Bajaj, Varun; Mack, J.; Marinelli, Mariarosa; Medina, J.; Pidgeon, A.; Kozhurina-Platais, V.; Shanahan, Clare; Som, Debopam

doi:10.3847/1538-3881/ac73f0

Cited by 21 publications

(14 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In each orbit, images were collected at several exposure levels, in which the central core of Didymos was unsaturated in short exposures and long exposures saturated Didymos to image the relatively faint ejecta and tail. All images were collected through filter F350LP (pivot wavelength 587 nm, bandwidth 149 nm) 30 .…”

Section: Methodsmentioning

confidence: 99%

Ejecta from the DART-produced active asteroid Dimorphos

Hirabayashi

Farnham

et al. 2023

Nature

View full text Add to dashboard Cite

Some active asteroids have been proposed to be formed as a result of impact events1. Because active asteroids are generally discovered by chance only after their tails have fully formed, the process of how impact ejecta evolve into a tail has, to our knowledge, not been directly observed. The Double Asteroid Redirection Test (DART) mission of NASA2, in addition to having successfully changed the orbital period of Dimorphos3, demonstrated the activation process of an asteroid resulting from an impact under precisely known conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope from impact time T + 15 min to T + 18.5 days at spatial resolutions of around 2.1 km per pixel. Our observations reveal the complex evolution of the ejecta, which are first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and subsequently by solar radiation pressure. The lowest-speed ejecta dispersed through a sustained tail that had a consistent morphology with previously observed asteroid tails thought to be produced by an impact4,5. The evolution of the ejecta after the controlled impact experiment of DART thus provides a framework for understanding the fundamental mechanisms that act on asteroids disrupted by a natural impact1,6.

show abstract

Section: Methodsmentioning

confidence: 99%

Ejecta from the DART-produced active asteroid Dimorphos

Hirabayashi

Farnham

et al. 2023

Nature

View full text Add to dashboard Cite

show abstract

“…For context, all HST ZPs were defined in units of AB-mag for a count rate of 1.000 e − pixel −1 s −1 . This definition permitted monitoring of the ZPs' wavelength and time dependence over many decades (e.g., Calamida et al 2022;Windhorst et al 2011Windhorst et al , 2022. (For a summary, see Section 4 and references therein of Windhorst et al 2022.…”

Section: First Assessment Of Calibration Qualitymentioning

confidence: 99%

JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

Windhorst

Cohen

Jansen

et al. 2022

View full text Add to dashboard Cite

We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST “Prime Extragalactic Areas for Reionization and Lensing Science” (PEARLS) project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP); seven gravitationally lensing clusters; two high redshift protoclusters; and the iconic backlit VV 191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, active galactic nucleus (AGN) growth, and First Light. Five fields—the JWST NEP Time-Domain Field (TDF), IRAC Dark Field, and three lensing clusters—will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9–4.5 μm galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9–4.5 μm. PEARLS is designed to be of lasting benefit to the community.

show abstract

“…The absolute flux calibration is determined by the calwf3 data-processing pipeline, which produces the calibrated single-visit files (FLCs) that are combined during the drizzle process (Section 3). The HST instruments are exceptionally well characterized, and details of the calwf3 calibrations are described in Section 3 of the Instrument Handbook (Sahu 2021) and Calamida et al (2022). The flux and magnitude values reported for each filter include the isophotal (ISO) and automatic (AUTO) aperture measurements.…”

Section: Photometric Catalogmentioning

confidence: 99%

The MUSE Ultra Deep Field (MUDF). III. Hubble Space Telescope WFC3 Grism Spectroscopy and Imaging

Revalski

Rafelski

Fumagalli

et al. 2023

ApJS

View full text Add to dashboard Cite

We present extremely deep Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations of the MUSE Ultra Deep Field. This unique region of the sky contains two quasars at z ≈ 3.22 that are separated by only ∼500 kpc, providing a stereoscopic view of gas and galaxies in emission and absorption across ∼10 billion years of cosmic time. We have obtained 90 orbits of HST WFC3 G141 near-infrared grism spectroscopy of this field in a single pointing, as well as 142 hr of optical spectroscopy with the Very Large Telescope Multi Unit Spectroscopic Explorer (MUSE). The WFC3 (F140W, F125W, and F336W) and archival WFPC2 (F702W and F450W) imaging provides five-filter photometry that we use to detect 3375 sources between z ≈ 0–6, including 1536 objects in a deep central pointing with both spectroscopic and photometric coverage. The F140W and F336W mosaics reach exceptional depths of m AB ≈ 28 and 29, respectively, providing near-infrared and rest-frame ultraviolet information for 1580 sources, and we reach 5σ continuum detections for objects as faint as m AB ≈ 27 in the grism spectra. The extensive wavelength coverage of MUSE and WFC3 allows us to measure spectroscopic redshifts for 419 sources, down to galaxy stellar masses of log(M/M ⊙) ≈7 at z ≈ 1–2. In this publication, we provide the calibrated HST data and source catalogs as High Level Science Products for use by the community, which includes photometry, morphology, and redshift measurements that enable a variety of studies aimed at advancing our models of galaxy formation and evolution in different environments.

show abstract

New Photometric Calibration of the Wide Field Camera 3 Detectors

Cited by 21 publications

References 15 publications

Ejecta from the DART-produced active asteroid Dimorphos

Ejecta from the DART-produced active asteroid Dimorphos

JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

The MUSE Ultra Deep Field (MUDF). III. Hubble Space Telescope WFC3 Grism Spectroscopy and Imaging

Contact Info

Product

Resources

About