The Spitzer/IRAC Legacy over the GOODS Fields: Full-depth 3.6, 4.5, 5.8, and 8.0 μm Mosaics and Photometry for >9000 Galaxies at z ∼ 3.5–10 from the GOODS Reionization Era Wide-area Treasury from Spitzer (GREATS)

2021 ◽  
Vol 257 (2) ◽  
pp. 68
Author(s):  
Mauro Stefanon ◽  
Ivo Labbé ◽  
Pascal A. Oesch ◽  
Stephane De Barros ◽  
Valentino Gonzalez ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Point Sources ◽  
Wide Area ◽  
Tangential Plane ◽  
Point Spread Functions ◽  
James Webb Space Telescope ◽  
Deep Survey ◽  
Empirical Point ◽  
Galaxy Assembly

Abstract We present the deepest Spitzer/InfraRed Array Camera (IRAC) 3.6, 4.5, 5.8, and 8.0 μm wide-area mosaics yet over the Great Observatories Origins Deep Survey (GOODS)-N and GOODS-S fields as part of the GOODS Reionization Era wide-Area Treasury from Spitzer (GREATS) project. We reduced and mosaicked in a self-consistent way observations taken by the 11 different Spitzer/IRAC programs over the two GOODS fields from 12 yr of Spitzer cryogenic and warm-mission data. The cumulative depth in the 3.6 μm and 4.5 μm bands amounts to ∼4260 hr, ∼1220 hr of which are new very deep observations from the GREATS program itself. In the deepest area, the full-depth mosaics reach ≳200 hr over an area of ∼100 arcmin2, corresponding to a sensitivity of ∼29 AB magnitude at 3.6 μm (1σ for point sources). Archival cryogenic 5.8 μm and 8.0 μm band data (a cumulative 976 hr) are also included in the release. The mosaics are projected onto the tangential plane of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey/GOODS at a 0.″3 pixel−1 scale. This paper describes the methodology enabling, and the characteristics of, the public release of the mosaic science images, the corresponding coverage maps in the four IRAC bands, and the empirical point-spread functions (PSFs). These PSFs enable mitigation of the source blending effects by taking into account the complex position-dependent variation in the IRAC images. The GREATS data products are in the Infrared Science Archive. We also release the deblended 3.6–8.0 μm photometry 9192 Lyman-break galaxies at z ∼ 3.5–10. GREATS will be the deepest mid-infrared imaging until the James Webb Space Telescope and, as such, constitutes a major resource for characterizing early galaxy assembly.

The Phoenix Deep Survey: Optical and Near‐infrared Imaging Catalogs

2004 ◽  
Vol 155 (1) ◽  
pp. 1-13 ◽  
Author(s):  
M. Sullivan ◽  
A. M. Hopkins ◽  
J. Afonso ◽  
A. Georgakakis ◽  
B. Chan ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Near Infrared Imaging ◽  
Deep Survey ◽  
The Phoenix

scholarly journals The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging

2004 ◽  
Vol 600 (2) ◽  
pp. L93-L98 ◽  
Author(s):  
M. Giavalisco ◽  
H. C. Ferguson ◽  
A. M. Koekemoer ◽  
M. Dickinson ◽  
D. M. Alexander ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Near Infrared Imaging ◽  
Deep Survey ◽  
Initial Results

scholarly journals Maximizing the power of deep extragalactic imaging surveys with the James Webb Space Telescope

2019 ◽  
Vol 486 (3) ◽  
pp. 3087-3104 ◽  
Author(s):  
T W Kemp ◽  
J S Dunlop ◽  
R J McLure ◽  
C Schreiber ◽  
A C Carnall ◽  
...  
Keyword(s):  
Galaxy Evolution ◽  
Parallel Imaging ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Current Knowledge ◽  
Signal To Noise Ratio ◽  
Added Value ◽  
Space Telescope ◽  
James Webb Space Telescope ◽  
The Impact

Abstract We present a new analysis of the potential power of deep, near-infrared, imaging surveys with the James Webb Space Telescope (JWST) to improve our knowledge of galaxy evolution. In this work we properly simulate what can be achieved with realistic survey strategies, and utilize rigorous signal-to-noise ratio calculations to calculate the resulting posterior constraints on the physical properties of galaxies. We explore a broad range of assumed input galaxy types (>20 000 models, including extremely dusty objects) across a wide redshift range (out to z ≃ 12), while at the same time considering a realistic mix of galaxy properties based on our current knowledge of the evolving population (as quantified through the Empirical Galaxy Generator). While our main focus is on imaging surveys with NIRCam, spanning $\lambda _{\mathrm{ obs}} = 0.8\!-\!5.0\, \mu$m, an important goal of this work is to quantify the impact/added-value of: (i) parallel imaging observations with MIRI at longer wavelengths, and (ii) deeper supporting optical/UV imaging with HST (potentially prior to JWST launch) in maximizing the power and robustness of a major extragalactic NIRCam survey. We show that MIRI parallel 7.7-$\mu$m imaging is of most value for better constraining the redshifts and stellar masses of the dustiest (AV > 3) galaxies, while deep B-band imaging (reaching ≃ 28.5 AB mag) with ACS on HST is vital for determining the redshifts of the large numbers of faint/low-mass, z < 5 galaxies that will be detected in a deep JWST NIRCam survey.

scholarly journals An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies

2021 ◽  
Vol 502 (3) ◽  
pp. 3426-3435
Author(s):  
Ian Smail ◽  
U Dudzevičiūtė ◽  
S M Stach ◽  
O Almaini ◽  
J E Birkin ◽  
...  
Keyword(s):  
Star Formation ◽  
Surface Density ◽  
Near Infrared ◽  
Infrared Imaging ◽  
High Redshift ◽  
Formation Rate ◽  
High Attenuation ◽  
Deep Survey ◽  
Stellar Masses ◽  
Dust Attenuation

ABSTRACT We analyse a robust sample of 30 near-infrared-faint (KAB > 25.3, 5σ) submillimetre galaxies (SMGs) selected from a 0.96 deg2 field to investigate their properties and the cause of their faintness in optical/near-infrared wavebands. Our analysis exploits precise identifications based on Atacama Large Millimeter Array (ALMA) 870-μm continuum imaging, combined with very deep near-infrared imaging from the UKIDSS Ultra Deep Survey. We estimate that SMGs with KAB > 25.3 mag represent 15 ± 2 per cent of the total population brighter than S870 = 3.6 mJy, with a potential surface density of ∼450 deg−2 above S870 ≥ 1 mJy. As such, they pose a source of contamination in surveys for both high-redshift ‘quiescent’ galaxies and very high redshift Lyman-break galaxies. We show that these K-faint SMGs represent the tail of the broader submillimetre population, with comparable dust and stellar masses to KAB ≤ 25.3 mag SMGs, but lying at significantly higher redshifts (z = 3.44 ± 0.06 versus z = 2.36 ± 0.11) and having higher dust attenuation (AV = 5.2 ± 0.3 versus AV = 2.9 ± 0.1). We investigate the origin of the strong dust attenuation and find indications that these K-faint galaxies have smaller dust continuum sizes than the KAB ≤ 25.3 mag galaxies, as measured by ALMA, which suggests their high attenuation is related to their compact sizes. We identify a correlation of dust attenuation with star formation rate surface density (ΣSFR), with the K-faint SMGs representing the higher ΣSFR and highest AV galaxies. The concentrated, intense star formation activity in these systems is likely to be associated with the formation of spheroids in compact galaxies at high redshifts, but as a result of their high obscuration these galaxies are completely missed in ultraviolet, optical, and even near-infrared surveys.

scholarly journals MOIRCS Deep Survey. IX. Deep Near-Infrared Imaging Data and Source Catalog

2011 ◽  
Vol 63 (sp2) ◽  
pp. S379-S401 ◽  
Author(s):  
Masaru Kajisawa ◽  
Takashi Ichikawa ◽  
Ichi Tanaka ◽  
Toru Yamada ◽  
Masayuki Akiyama ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Imaging Data ◽  
Near Infrared Imaging ◽  
Deep Survey

scholarly journals Airborne methane remote measurements reveal heavy-tail flux distribution in Four Corners region

2016 ◽  
Vol 113 (35) ◽  
pp. 9734-9739 ◽  
Author(s):  
Christian Frankenberg ◽  
Andrew K. Thorpe ◽  
David R. Thompson ◽  
Glynn Hulley ◽  
Eric Adam Kort ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Thermal Emission ◽  
Geographic Area ◽  
Point Sources ◽  
Imaging Spectrometer ◽  
Thermal Infrared Imaging ◽  
Four Corners ◽  
Remote Measurements ◽  
Total Point

Methane (CH4) impacts climate as the second strongest anthropogenic greenhouse gas and air quality by influencing tropospheric ozone levels. Space-based observations have identified the Four Corners region in the Southwest United States as an area of large CH4 enhancements. We conducted an airborne campaign in Four Corners during April 2015 with the next-generation Airborne Visible/Infrared Imaging Spectrometer (near-infrared) and Hyperspectral Thermal Emission Spectrometer (thermal infrared) imaging spectrometers to better understand the source of methane by measuring methane plumes at 1- to 3-m spatial resolution. Our analysis detected more than 250 individual methane plumes from fossil fuel harvesting, processing, and distributing infrastructures, spanning an emission range from the detection limit ∼ 2 kg/h to 5 kg/h through ∼ 5,000 kg/h. Observed sources include gas processing facilities, storage tanks, pipeline leaks, and well pads, as well as a coal mine venting shaft. Overall, plume enhancements and inferred fluxes follow a lognormal distribution, with the top 10% emitters contributing 49 to 66% to the inferred total point source flux of 0.23 Tg/y to 0.39 Tg/y. With the observed confirmation of a lognormal emission distribution, this airborne observing strategy and its ability to locate previously unknown point sources in real time provides an efficient and effective method to identify and mitigate major emissions contributors over a wide geographic area. With improved instrumentation, this capability scales to spaceborne applications [Thompson DR, et al. (2016) Geophys Res Lett 43(12):6571–6578]. Further illustration of this potential is demonstrated with two detected, confirmed, and repaired pipeline leaks during the campaign.

scholarly journals Observational properties of a general relativistic instability supernova from a primordial supermassive star

2021 ◽  
Vol 503 (1) ◽  
pp. 1206-1213
Author(s):  
Takashi J Moriya ◽  
Ke-Jung Chen ◽  
Kimihiko Nakajima ◽  
Nozomu Tominaga ◽  
Sergei I Blinnikov
Keyword(s):  
Black Holes ◽  
Near Infrared ◽  
Infrared Imaging ◽  
High Redshift ◽  
Plateau Phase ◽  
Infrared Images ◽  
High Redshift Galaxies ◽  
James Webb Space Telescope ◽  
General Relativistic ◽  
The Time Domain

ABSTRACT We present the expected observational properties of a general relativistic instability supernova (GRSN) from the 55 500 M⊙ primordial (Population III) star. Supermassive stars exceeding $10^4\, \mathrm{M}_\odot$ may exist in the early Universe. They are generally considered to collapse through the general relativistic instability to be seed black holes to form supermassive ($\sim 10^9\, \mathrm{M}_\odot$) black holes observed as high-redshift quasars. Some of them, however, may explode as GRSNe if the explosive helium burning unbinds the supermassive stars following the collapse triggered by the general relativistic instability. We perform the radiation hydrodynamics simulation of the GRSN starting shortly before the shock breakout. We find that the GRSN is characterized by a long-lasting (550 d) luminous ($1.5\times 10^{44}\, \mathrm{erg\, s^{-1}}$) plateau phase with the photospheric temperature of around 5000 K in the rest frame. The plateau phase lasts for decades when it appears at high redshifts and it will likely be observed as a persistent source in the future deep near-infrared imaging surveys. Especially, the near-infrared images reaching 29 AB magnitude that can be obtained by Galaxy and Reionization EXplorer (G-REX) and James Webb Space Telescope (JWST) allow us to identify GRSNe up to z ≃ 15. Deeper images enable us to discover GRSNe at even higher redshifts. Having extremely red colour, they can be distinguished from other persistent sources such as high-redshift galaxies by using colour information. We conclude that the deep near-infrared images are able to constrain the existence of GRSNe from the primordial supermassive stars in the Universe even without the time domain information.

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