scholarly journals Observations of the Near-Infrared Extragalactic Background Light

2001 ◽  
Vol 204 ◽  
pp. 87-100
Author(s):  
Toshio Matsumoto
Keyword(s):  
Large Scale ◽  
Near Infrared ◽  
High Redshift ◽  
Far Infrared ◽  
Zodiacal Light ◽  
Extragalactic Background Light ◽  
Background Light ◽  
Infrared Telescope ◽  
Total Energy Flux ◽  
Infrared Spectrometer

We searched for the near infrared extragalactic background light (IREBL) in data from the Near Infrared Spectrometer (NIRS) on the Infrared Telescope in Space (IRTS). After subtracting the contribution of faint stars and a modeled zodiacal component, a significant isotropic emission is detected whose in-band flux amounts to ~ 30 nWm−2sr−1. This brightness is consistent with upper limits of COBE/DIRBE, but is significantly brighter than the integrated light of faint galaxies. The star subtraction analyses from DIRBE data show essentially the same results apart from the uncertainty in the model of the zodiacal light. A significant fluctuation of the sky brightness was also detected. A 2-point correlation analysis indicates that the fluctuations have a characteristic spatial structure of 100 ~ 200 arcmin. This could be an indication of the large scale structure at high redshift. Combined with the far infrared and submillimeter EBL, the total energy flux amounts to 50 ~ 80 nWm−2sr−1 which is so bright that unknown energy sources at high redshifts are required.

scholarly journals Large angular scale fluctuations of near-infrared extragalactic background light based on the IRTS observations

2019 ◽  
Vol 71 (4) ◽  
Author(s):  
Min Gyu Kim ◽  
Toshio Matsumoto ◽  
Hyung Mok Lee ◽  
Woong-Seob Jeong ◽  
Kohji Tsumura ◽  
...  
Keyword(s):  
Large Scale ◽  
Near Infrared ◽  
High Redshift ◽  
Zodiacal Light ◽  
Extragalactic Background Light ◽  
Background Light ◽  
Normal Galaxies ◽  
Infrared Telescope ◽  
Angular Scale ◽  
Using Data

Abstract We measure the spatial fluctuations of the Near-Infrared Extragalactic Background Light (NIREBL) from 2° to 20° in angular scale at the 1.6 and $2.2\, \mu \mathrm{m}$ using data obtained with Near-Infrared Spectrometer (NIRS) on board the Infrared Telescope in Space (IRTS). The brightness of the NIREBL is estimated by subtracting foreground components such as zodiacal light, diffuse Galactic light, and integrated star light from the observed sky. The foreground components are estimated using well-established models and archive data. The NIREBL fluctuations for the 1.6 and $2.2\, \mu \mathrm{m}$ connect well toward the sub-degree scale measurements from previous studies. Overall, the fluctuations show a wide bump with a center at around 1° and the power decreases toward larger angular scales with nearly a single power-law spectrum (i.e., ${F[\sqrt{l(l+1)C_l/2\pi }]} \sim \theta ^{-1}]$, indicating that the large-scale power is dominated by the random spatial distribution of the sources. After examining several known sources, contributors such as normal galaxies, high-redshift objects, intra-halo light, and far-IR cosmic background, we conclude that the excess fluctuation at around the 1° scale cannot be explained by any of them.

scholarly journals Infrared Extragalactic Background Light

1990 ◽  
Vol 139 ◽  
pp. 317-326
Author(s):  
Toshio Matsumoto
Keyword(s):  
Near Infrared ◽  
Background Radiation ◽  
High Redshift ◽  
Dust Emission ◽  
Far Infrared ◽  
Cosmic Background Radiation ◽  
Infrared Region ◽  
Clear Correlation ◽  
Extragalactic Background Light ◽  
Background Light

Infrared extragalactic background light plays an important role in the study of the early history of the universe, especially as a probe to search for the primeval galaxies. In the near-infrared region, UV and visible light emitted from high redshift galaxies could be observable. Measurement of the sky fluctuation at 2.2 μm gives a very low upper limit. The rocket observation of the near-infrared diffuse emission reveals isotropic emission which is possibly ascribed to an extragalactic origin. The observed brightness and fluctuation are not consistent with the standard scenario of the primeval galaxies. In the far-infrared region, integrated light of dust emission of the distant galaxies forms another cosmic background radiation. IRAS and the Nagoya-Berkeley rocket experiment found a clear correlation between HI column density and far-infrared sky brightness; however, there remains an uncorrelated isotropic emission component. If we ascribe this emission to extragalactic origin, a fairly big evolution effect is required. In the submillimeter region, excess emission over the 2.74K blackbody spectrum was found, which requires the vast energy generation in the early universe.

Infrared Telescope in Space Observations of the Near‐Infrared Extragalactic Background Light

2005 ◽  
Vol 626 (1) ◽  
pp. 31-43 ◽  
Author(s):  
T. Matsumoto ◽  
S. Matsuura ◽  
H. Murakami ◽  
M. Tanaka ◽  
M. Freund ◽  
...  
Keyword(s):  
Near Infrared ◽  
Extragalactic Background Light ◽  
Background Light ◽  
Infrared Telescope ◽  
Space Observations

scholarly journals Mapping large-scale-structure evolution over cosmic times

2021 ◽  
Author(s):  
Marta B. Silva ◽  
Ely D. Kovetz ◽  
Garrett K. Keating ◽  
Azadeh Moradinezhad Dizgah ◽  
Matthieu Bethermin ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Large Scale ◽  
High Redshift ◽  
Formation Rate ◽  
Far Infrared ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Structure Evolution ◽  
Intensity Mapping ◽  
Wide Range

AbstractThis paper outlines the science case for line-intensity mapping with a space-borne instrument targeting the sub-millimeter (microwaves) to the far-infrared (FIR) wavelength range. Our goal is to observe and characterize the large-scale structure in the Universe from present times to the high redshift Epoch of Reionization. This is essential to constrain the cosmology of our Universe and form a better understanding of various mechanisms that drive galaxy formation and evolution. The proposed frequency range would make it possible to probe important metal cooling lines such as [CII] up to very high redshift as well as a large number of rotational lines of the CO molecule. These can be used to trace molecular gas and dust evolution and constrain the buildup in both the cosmic star formation rate density and the cosmic infrared background (CIB). Moreover, surveys at the highest frequencies will detect FIR lines which are used as diagnostics of galaxies and AGN. Tomography of these lines over a wide redshift range will enable invaluable measurements of the cosmic expansion history at epochs inaccessible to other methods, competitive constraints on the parameters of the standard model of cosmology, and numerous tests of dark matter, dark energy, modified gravity and inflation. To reach these goals, large-scale structure must be mapped over a wide range in frequency to trace its time evolution and the surveyed area needs to be very large to beat cosmic variance. Only a space-borne mission can properly meet these requirements.

scholarly journals Fitting Zodiacal Models

2001 ◽  
Vol 204 ◽  
pp. 157-160 ◽  
Author(s):  
Edward L. Wright
Keyword(s):  
Solar System ◽  
Radiation Field ◽  
Measured Data ◽  
Low Earth Orbit ◽  
Earth Orbit ◽  
Zodiacal Light ◽  
Extragalactic Background Light ◽  
Background Light

Models of the zodiacal light are necessary to convert measured data taken from low Earth orbit into the radiation field outside the Solar System. The uncertainty in these models dominates the overall uncertainty in determining the extragalactic background light for wavelengths λ < 100 μm.

scholarly journals Near-Infrared Images of the Serpens Molecular Cloud Core

1989 ◽  
Vol 120 ◽  
pp. 227-230
Author(s):  
C. Eiroa ◽  
M. Casali
Keyword(s):  
Molecular Cloud ◽  
Large Scale ◽  
Near Infrared ◽  
Far Infrared ◽  
Infrared Images ◽  
Infrared Source ◽  
Stellar Objects ◽  
Dark Clouds ◽  
First Time ◽  
Cloud Core

ABSTRACT:Near-infrared images of the Serpens molecular cloud core have been carried out at UKIRT (Mauna Kea Observatory) using the infrared array camera, IRCAM. A large-scale diffuse nebulosity extending over the central part of the core is observed. Over 100 K-sources are detected in the 30 arc min2 cloud core. Some of them are PMS objects which were previously unknown. For the first time, a near-infrared counterpart of the far-infrared source Seroens FIRS1 has been detected. The 2.2 µm source appears as a point like object at the apex of an extended knotty, jet-like nebulosity oriented towards the northwest. In addition, a group of 11 stellar objects is seen in the position of the IR/radio source SVS4. These objects are embedded in a very faint nebulosity and form one of the densest clustering of young stars found in dark clouds.

High efficiency near infrared spectrometer for zodiacal light spectral study

2008 ◽  
Author(s):  
A. S. Kutyrev ◽  
R. Arendt ◽  
E. Dwek ◽  
S. H. Moseley ◽  
D. Rapchun ◽  
...  
Keyword(s):  
Spectral Study ◽  
Near Infrared ◽  
High Efficiency ◽  
Zodiacal Light ◽  
Infrared Spectrometer ◽  
Near Infrared Spectrometer

scholarly journals Physics of a clumpy lensed galaxy at z = 1.6

2018 ◽  
Vol 619 ◽  
pp. A15 ◽  
Author(s):  
M. Girard ◽  
M. Dessauges-Zavadsky ◽  
D. Schaerer ◽  
J. Richard ◽  
K. Nakajima ◽  
...  
Keyword(s):  
Star Formation ◽  
Gravitational Lensing ◽  
Near Infrared ◽  
High Redshift ◽  
Formation Rate ◽  
Far Infrared ◽  
Rotating Disk ◽  
Cluster Galaxy ◽  
Star Forming ◽  
The Galaxy

Observations have shown that massive star-forming clumps are present in the internal structure of high-redshift galaxies. One way to study these clumps in detail with a higher spatial resolution is by exploiting the power of strong gravitational lensing which stretches images on the sky. In this work, we present an analysis of the clumpy galaxy A68-HLS115 at z = 1.5858, located behind the cluster Abell 68, but strongly lensed by a cluster galaxy member. Resolved observations with SINFONI/VLT in the near-infrared (NIR) show Hα, Hβ, [NII], and [OIII] emission lines. Combined with images covering the B band to the far-infrared (FIR) and CO(2–1) observations, this makes this galaxy one of the only sources for which such multi-band observations are available and for which it is possible to study the properties of resolved star-forming clumps and to perform a detailed analysis of the integrated properties, kinematics, and metallicity. We obtain a stability of υrot/σ0 = 2.73 by modeling the kinematics, which means that the galaxy is dominated by rotation, but this ratio also indicates that the disk is marginally stable. We find a high intrinsic velocity dispersion of 80 ± 10 km s−1 that could be explained by the high gas fraction of fgas = 0.75 ± 0.15 observed in this galaxy. This high fgas and the observed sSFR of 3.12 Gyr−1 suggest that the disk turbulence and instabilities are mostly regulated by incoming gas (available gas reservoir for star formation). The direct measure of the Toomre stability criterion of Qcrit = 0.70 could also indicate the presence of a quasi-stable thick disk. Finally, we identify three clumps in the Hα map which have similar velocity dispersions, metallicities, and seem to be embedded in the rotating disk. These three clumps contribute together to ∼40% on the SFRHα of the galaxy and show a star formation rate density about ∼100 times higher than HII regions in the local Universe.

Sign in / Sign up

Export Citation Format

Share Document