An official website of the United States government
ABSTRACT We present a mock image catalogue of ∼100 000 MUV ≃ −22.5 to −19.6 mag galaxies at z = 7–12 from the bluetides cosmological simulation. We create mock images of each galaxy with the James Webb Space Telescope (JWST), Hubble, Roman, and Euclid Space Telescopes, as well as Subaru, and VISTA, with a range of near- and mid-infrared filters. We perform photometry on the mock images to estimate the success of these instruments for detecting high-z galaxies. We predict that JWST will have unprecedented power in detecting high-z galaxies, with a 95 per cent completeness limit at least 2.5 mag fainter than VISTA and Subaru, 1.1 mag fainter than Hubble, and 0.9 mag fainter than Roman, for the same wavelength and exposure time. Focusing on JWST, we consider a range of exposure times and filters, and find that the NIRCam F356W and F277W filters will detect the faintest galaxies, with 95 per cent completeness at m ≃ 27.4 mag in 10-ks exposures. We also predict the number of high-z galaxies that will be discovered by upcoming JWST imaging surveys. We predict that the COSMOS-Web survey will detect ∼1000 M1500 Å < −20.1 mag galaxies at 6.5 < z < 7.5, by virtue of its large survey area. JADES-Medium will detect almost $$100{{\ \rm per\ cent}}$$ of M1500 Å ≲ −20 mag galaxies at z < 8.5 due to its significant depth, however, with its smaller survey area it will detect only ∼100 of these galaxies at 6.5 < z < 7.5. Cosmic variance results in a large range in the number of predicted galaxies each survey will detect, which is more evident in smaller surveys such as CEERS and the PEARLS NEP and GOODS-S fields.
more »
« less
This content will become publicly available on September 19, 2026
NIR Filter Transformations Across the HR Diagram: JWST, Roman, and Euclid
We present new color transformations between select near-infrared filters on JWST/NIRCam, Euclid/NISP, Roman/WFI, HST, and ground-basedizY+IJHKS, for a total of 105 unique filter combinations. Additionally, we apply these transformations to predict the color–magnitude relation of the tip of the red giant branch as seen with JWST, Euclid, and Roman based on theoretical results for Hubble Space Telescope and Two Micron All Sky Survey filters; for JWST we find good agreement with empirical results in the literature. We also find typical residual dispersion around these transformations of 0.01 mag for Cepheid and RR Lyrae variables and RGB stars, but up to 0.1 mag for O- and C-rich TP-AGB stars.
more »
« less
- PAR ID:
- 10654766
- Publisher / Repository:
- American Astronomical Society Journals
- Date Published:
- Journal Name:
- The Astronomical Journal
- Volume:
- 170
- Issue:
- 4
- ISSN:
- 0004-6256
- Page Range / eLocation ID:
- 232
- Subject(s) / Keyword(s):
- Calibration Photometric systems Near infrared astronomy Stellar colors Stellar populations 2179 1233 1093 1590 1622 Instrumentation and Methods for Astrophysics
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
More Like this
-
-
Abstract About 70 luminous quasars discovered atz> 6.5 are strongly biased toward the bright end, thus not providing a comprehensive view of quasar abundance beyond the cosmic dawn. We present the predicted results of the Roman/Rubin high-redshift quasar survey, yielding 3 times more, 2–4 mag deeper quasar samples, probing high-redshift quasars across a broad range of luminosities, especially faint quasars atLbol∼ 1010L⊙orM1450∼ −22, which are currently poorly explored. We include high-zquasars, galactic dwarfs, and low-zcompact galaxies with similar colors as quasar candidates. We create mock catalogs based on population models to evaluate selection completeness and efficiency. We utilize the classical color dropout method in thezandYbands to select primary quasar candidates, followed up with the Bayesian selection method to identify quasars. We show that overall selection completeness >80% and efficiency ∼10% at 6.5 <z< 9, with 180 quasars atz> 6.5, 20 atz> 7.5, and 2 atz> 8.5. The quasar yields depend sensitively on the assumed quasar luminosity shape and redshift evolution. Brown dwarf rejection through proper motion up to 50% can be made for stars brighter than 25 mag, low-zgalaxies dominate at fainter magnitude. Our results show that Roman/Rubin are able to discover a statistical sample of the earliest and faintest quasars in the Universe. The new valuable data sets are worth follow-up studies with JWST and Extremely Large Telescopes to determine the quasar luminosity function faint end slope and constraint the supermassive black holes growth in the early Universe.more » « less
-
Abstract Hot DA white dwarfs (DAWDs) have fully radiative pure hydrogen atmospheres that are the least complicated to model. Pulsationally stable, they are fully characterized by their effective temperatureTeffand surface gravity , which can be deduced from their optical spectra and used in model atmospheres to predict their spectral energy distributions (SEDs). Based on this, three bright DAWDs have defined the spectrophotometric flux scale of the CALSPEC system of the Hubble Space Telescope (HST). In this paper we add 32 new fainter (16.5 <V< 19.5) DAWDs spread over the whole sky and within the dynamic range of large telescopes. Using ground-based spectra and panchromatic photometry with HST/WFC3, a new hierarchical analysis process demonstrates consistency between model and observed fluxes above the terrestrial atmosphere to <0.004 mag rms from 2700 to 7750 Å and to 0.008 mag rms at 1.6μm for the total set of 35 DAWDs. These DAWDs are thus established as spectrophotometric standards with unprecedented accuracy from the near-ultraviolet to the near-infrared, suitable for both ground- and space-based observatories. They are embedded in existing surveys like the Sloan Digital Sky Survey, Pan-STARRS, and Gaia, and will be naturally included in the Large Synoptic Survey Telescope survey by the Rubin Observatory. With additional data and analysis to extend the validity of their SEDs further into the infrared, these spectrophotometric standard stars could be used for JWST, as well as for the Roman and Euclid observatories.more » « less
-
Understanding the detailed properties of stars in the infrared is of critical importance with new missions focusing on the infrared (JWST, Roman). The ground-based wide-field infrared instrument, FourStar, on the Magellan telescope contains a number of medium band filters that are optimized for photometric redshifts, but also provide nearly continuous spectral coverage for stars. These filters, however, lack absolute calibration. In this project, we adapted a technique used for galaxies to be used for stars. We used multi-band photometry to fit a likely SED model to each star and then generated synthetic photometry from the SED model to produce the magnitude of the star in a given filter. Statistically, we then determined the zero point in each filter in each image. This will be used to calibrate a large survey aiming to better understand near-infrared properties of stars for application to the extragalactic distance scale (with JWST and Roman).more » « less
-
Understanding the detailed properties of stars in the infrared is of critical importance with new missions focusing on the infrared (JWST, Roman). The ground-based wide-field infrared instrument, FourStar, on the Magellan telescope contains a number of medium band filters that are optimized for photometric redshifts, but also provide nearly continuous spectral coverage for stars. These filters, however, lack absolute calibration. In this project, we adapted a technique used for galaxies to be used for stars. We used multi-band photometry to fit a likely SED model to each star and then generated synthetic photometry from the SED model to produce the magnitude of the star in a given filter. Statistically, we then determined the zero point in each filter in each image. This will be used to calibrate a large survey aiming to better understand near-infrared properties of stars for application to the extragalactic distance scale (with JWST and Roman).more » « less
