96 research outputs found
IoT protocols, architectures, and applications
The proliferation of embedded systems, wireless technologies, and Internet protocols have made it possible for the Internet-of-things (IoT) to bridge the gap between the physical and the virtual world and thereby enabling monitoring and control of the physical environment by data processing systems. IoT refers to the inter-networking of everyday objects that are equipped with sensing, computing, and communication capabilities. These networks can collaborate to autonomously solve a variety of tasks. Due to the very diverse set of applications and application requirements, there is no single communication technology that is able to provide cost-effective and close to optimal performance in all scenarios. In this chapter, we report on research carried out on a selected number of IoT topics: low-power wide-area networks, in particular, LoRa and narrow-band IoT (NB-IoT); IP version 6 over IEEE 802.15.4 time-slotted channel hopping (6TiSCH); vehicular antenna design, integration, and processing; security aspects for vehicular networks; energy efficiency and harvesting for IoT systems; and software-defined networking/network functions virtualization for (SDN/NFV) IoT
Probing the earliest phases in the formation of massive galaxies with simulated HST+JWST imaging data from Illustris
We use the Illustris-1 simulation to explore the capabilities of the
and data to analyze the
stellar populations in high-redshift galaxies, taking advantage of the combined
depth, spatial resolution, and wavelength coverage. For that purpose, we use
simulated broad-band ACS, WFC3 and NIRCam data and 2-dimensional stellar
population synthesis (2D-SPS) to derive the integrated star formation history
(SFH) of massive (MM) simulated galaxies at
M galaxy. In
particular, we explore the potential of HST and JWST datasets reaching a depth
similar to those of the CANDELS and ongoing CEERS observations, respectively,
and concentrate on determining the capabilities of this dataset for
characterizing the first episodes in the SFH of local
MM galaxies by studying their progenitors at
. The 2D-SPS method presented in this paper has been calibrated to
robustly recover the cosmic times when the first star formation episodes
occurred in massive galaxies, i.e., the first stages in their integrated SFHs.
In particular, we discuss the times when the first 1% to 50% of their total
stellar mass formed in the simulation. We demonstrate that we can recover these
ages with typical median systematic offset of less than 5% and scatter around
20%-30%. According to our measurements on Illustris data, we are able to
recover that local MM galaxies would have started
their formation by , forming the first 5% of their stellar mass present
at by , 10% by , and 25% by .Comment: 28 pages, 13 figures, 4 tables. ApJ in press. Summary of changes from
original submission: the major change is that we now include in Sec. 6 the
comparison of the results obtained for our sample of massive 1 < z < 4
progenitors with those obtained by considering all massive galaxies at 1 < z
< 4 in the simulated images. Several figures and sections have been update
CEERS: Diversity of Lyman-Alpha Emitters during the Epoch of Reionization
We analyze rest-frame ultraviolet to optical spectra of three -
galaxies whose Ly-emission lines were previously detected with
Keck/MOSFIRE observations, using the JWST/NIRSpec observations from the Cosmic
Evolution Early Release Science (CEERS) survey. From NIRSpec data, we confirm
the systemic redshifts of these Ly emitters, and emission-line ratio
diagnostics indicate these galaxies were highly ionized and metal poor. We
investigate Ly line properties, including the line flux, velocity
offset, and spatial extension. For the one galaxy where we have both NIRSpec
and MOSFIRE measurements, we find a significant offset in their flux
measurements ( greater in MOSFIRE) and a marginal difference in
the velocity shifts. The simplest interpretation is that the Ly
emission is extended and not entirely encompassed by the NIRSpec slit. The
cross-dispersion profiles in NIRSpec reveal that Ly in one galaxy is
significantly more extended than the non-resonant emission lines. We also
compute the expected sizes of ionized bubbles that can be generated by the
Ly sources, discussing viable scenarios for the creation of sizable
ionized bubbles (1 physical Mpc). The source with the highest-ionization
condition is possibly capable of ionizing its own bubble, while the other two
do not appear to be capable of ionizing such a large region, requiring
additional sources of ionizing photons. Therefore, the fact that we detect
Ly from these galaxies suggests diverse scenarios on escape of
Ly during the epoch of reionization. High spectral resolution spectra
with JWST/NIRSpec will be extremely useful for constraining the physics of
patchy reionization.Comment: Submitted to ApJ (18 pages, 7 figures, 2 tables
CEERS Key Paper VII: Emission Line Ratios from NIRSpec and NIRCam Wide-Field Slitless Spectroscopy at z>2
We use James Webb Space Telescope Near-Infrared Camera Wide Field Slitless
Spectroscopy (NIRCam WFSS) and Near-Infrared spectrograph (NIRSpec) in the
Cosmic Evolution Early Release survey (CEERS) to measure rest-frame optical
emission-line of 155 galaxies at z>2. The blind NIRCam grism observations
include a sample of galaxies with bright emission lines that were not observed
on the NIRSpec masks. We study the changes of the Ha, [OIII]/Hb, and
[NeIII]/[OII] emission lines in terms of redshift by comparing to lower
redshift SDSS and CLEAR samples. We find a significant (>3) correlation
between [OIII]/Hb with redshift, while [NeIII]/[OII] has a marginal (2)
correlation with redshift. We compare [OIII]/Hb and [NeIII]/[OII] to stellar
mass and Hb SFR. We find that both emission-line ratios have a correlation with
Hb SFR and an anti-correlation with stellar mass across the redshifts 0<z<9.
Comparison with MAPPINGS~V models indicates that these trends are consistent
with lower metallicity and higher ionization in low-mass and high-SFR galaxies.
We additionally compare to IllustriousTNG predictions and find that they
effectively describe the highest [OIII]/Hb ratios observed in our sample,
without the need to invoke MAPPINGS models with significant shock ionizionation
components.Comment: 16 pages, 11 figure
Spectroscopic verification of very luminous galaxy candidates in the early universe
During the first 500 million years of cosmic history, the first stars and
galaxies formed and seeded the cosmos with heavy elements. These early galaxies
illuminated the transition from the cosmic "dark ages" to the reionization of
the intergalactic medium. This transitional period has been largely
inaccessible to direct observation until the recent commissioning of JWST,
which has extended our observational reach into that epoch. Excitingly, the
first JWST science observations uncovered a surprisingly high abundance of
early star-forming galaxies. However, the distances (redshifts) of these
galaxies were, by necessity, estimated from multi-band photometry. Photometric
redshifts, while generally robust, can suffer from uncertainties and/or
degeneracies. Spectroscopic measurements of the precise redshifts are required
to validate these sources and to reliably quantify their space densities,
stellar masses, and star formation rates, which provide powerful constraints on
galaxy formation models and cosmology. Here we present the results of JWST
follow-up spectroscopy of a small sample of galaxies suspected to be amongst
the most distant yet observed. We confirm redshifts z > 10 for two galaxies,
including one of the first bright JWST-discovered candidates with z = 11.4, and
show that another galaxy with suggested z ~ 16 instead has z = 4.9, with strong
emission lines that mimic the expected colors of more distant objects. These
results reinforce the evidence for the rapid production of luminous galaxies in
the very young Universe, while also highlighting the necessity of spectroscopic
verification for remarkable candidates.Comment: Submitted to Natur
A Milky Way-like barred spiral galaxy at a redshift of 3
International audienceThe majority of massive disk galaxies in the local Universe show a stellar barred structure in their central regions, including our Milky Way. Bars are supposed to develop in dynamically cold stellar disks at low redshift, as the strong gas turbulence typical of disk galaxies at high redshift suppresses or delays bar formation. Moreover, simulations predict bars to be almost absent beyond in the progenitors of Milky Way-like galaxies. Here we report observations of ceers-2112, a barred spiral galaxy at redshift , which was already mature when the Universe was only 2 Gyr old. The stellar mass () and barred morphology mean that ceers-2112 can be considered a progenitor of the Milky Way, in terms of both structure and mass-assembly history in the first 2 Gyr of the Universe, and was the closest in mass in the first 4 Gyr. We infer that baryons in galaxies could have already dominated over dark matter at , that high-redshift bars could form in approximately 400 Myr and that dynamically cold stellar disks could have been in place by redshift (more than 12 Gyrs ago)
CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes
We present the mid-IR (MIR) morphologies for 64 star-forming galaxies at
0.210^{9}~M_\odot} using JWST MIRI
observations from the Cosmic Evolution Early Release Science survey (CEERS).
The MIRI bands span the MIR (7.7--21~m), enabling us to measure the
effective radii () and S\'{e}rsic indexes of these SFGs at
rest-frame 6.2 and 7.7 m, which contains strong emission from Polycyclic
aromatic hydrocarbon (PAH) features, a well-established tracer of star
formation in galaxies. We define a ``PAH-band'' as the MIRI bandpass that
contains these features at the redshift of the galaxy. We then compare the
galaxy morphologies in the PAH-bands to those in rest-frame Near-UV (NUV) using
HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging
from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of
(unobscured) massive stars and the stellar continuum, respectively. The
of galaxies in the PAH-band are slightly smaller (10\%)
than those in F160W for galaxies with at
, but the PAH-band and F160W have a similar fractions of light within
1 kpc. In contrast, the of galaxies in the NUV-band are larger,
with lower fractions of light within 1 kpc compared to F160W for galaxies at
. Using the MIRI data to estimate the surface
density, we find the correlation between the surface
density and stellar mass has a steeper slope than that of the
surface density and stellar mass, suggesting more massive
galaxies having increasing amounts of obscured fraction of star formation in
their inner regions. This paper demonstrates how the high-angular resolution
data from JWST/MIRI can reveal new information about the morphology of
obscured-star formation.Comment: 28 pages, 11 figures, Accepted by Ap
Extremely Red Galaxies at z = 5-9 with MIRI and NIRSpec:Dusty Galaxies or Obscured Active Galactic Nuclei?
We study a new population of extremely red objects (EROs) recently discovered by the James Webb Space Telescope (JWST) based on their NIRCam colors F277W − F444W > 1.5 mag. We find 37 EROs in the Cosmic Evolution Early Release Science Survey (CEERS) field with F444W < 28 mag and photometric redshifts between 5 < z < 7, with median z = 6.9 − 1.6 + 1.0 . Surprisingly, despite their red long-wavelength colors, these EROs have blue short-wavelength colors (F150W − F200W ∼ 0 mag) indicative of bimodal spectral energy distributions (SEDs) with a red, steep slope in the rest-frame optical, and a blue, flat slope in the rest-frame UV. Moreover, all these EROs are unresolved, point-like sources in all NIRCam bands. We analyze the SEDs of eight of them with MIRI and NIRSpec observations using stellar population models and active galactic nucleus (AGN) templates. We find that dusty galaxies or obscured AGNs provide similarly good SED fits but different stellar properties: massive and dusty, log M ⋆ / M ⊙ ∼ 10 and A V ≳ 3 mag, or low mass and obscured, log M ⋆ / M ⊙ ∼ 7.5 and A V ∼ 0 mag, hosting an obscured quasi-stellar object (QSO). SED modeling does not favor either scenario, but their unresolved sizes are more suggestive of AGNs. If any EROs are confirmed to have log M ⋆ / M ⊙ ≳ 10.5, it would increase the pre-JWST number density at z > 7 by up to a factor ∼60. Similarly, if they are QSOs with luminosities in the L bol > 1045-46 erg s−1 range, their number would exceed that of bright blue QSOs by more than three orders of magnitude. Additional photometry at mid-infrared wavelengths will reveal the true nature of the red continuum emission in these EROs and will place this puzzling population in the right context of galaxy evolution.</p
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