897 research outputs found
Reionization after Planck: the derived growth of the cosmic ionizing emissivity now matches the growth of the galaxy UV luminosity density
Thomson optical depth tau measurements from Planck provide new insights into
the reionization of the universe. In pursuit of model-independent constraints
on the properties of the ionising sources, we determine the empirical evolution
of the cosmic ionizing emissivity. We use a simple two-parameter model to map
out the evolution in the emissivity at z>~6 from the new Planck optical depth
tau measurements, from the constraints provided by quasar absorption spectra
and from the prevalence of Ly-alpha emission in z~7-8 galaxies. We find the
redshift evolution in the emissivity dot{N}_{ion}(z) required by the
observations to be d(log Nion)/dz=-0.15(-0.11)(+0.08), largely independent of
the assumed clumping factor C_{HII} and entirely independent of the nature of
the ionising sources. The trend in dot{N}_{ion}(z) is well-matched by the
evolution of the galaxy UV-luminosity density (dlog_{10}
rho_UV/dz=-0.11+/-0.04) to a magnitude limit >~-13 mag, suggesting that
galaxies are the sources that drive the reionization of the universe. The role
of galaxies is further strengthened by the conversion from the UV luminosity
density rho_UV to dot(N)_{ion}(z) being possible for physically-plausible
values of the escape fraction f_{esc}, the Lyman-continuum photon production
efficiency xi_{ion}, and faint-end cut-off to the luminosity
function. Quasars/AGN appear to match neither the redshift evolution nor
normalization of the ionizing emissivity. Based on the inferred evolution in
the ionizing emissivity, we estimate that the z~10 UV-luminosity density is
8(-4)(+15)x lower than at $z~6, consistent with the observations. The present
approach of contrasting the inferred evolution of the ionizing emissivity with
that of the galaxy UV luminosity density adds to the growing observational
evidence that faint, star-forming galaxies drive the reionization of the
universe.Comment: 20 pages, 12 figures, 5 tables, Astrophysical Journal, updated to
match version in press, Figure 6 shows the main result of the pape
A candidate redshift z ~ 10 galaxy and rapid changes in that population at an age of 500 Myr
Searches for very-high-redshift galaxies over the past decade have yielded a
large sample of more than 6,000 galaxies existing just 900-2,000 million years
(Myr) after the Big Bang (redshifts 6 > z > 3; ref. 1). The Hubble Ultra Deep
Field (HUDF09) data have yielded the first reliable detections of z ~ 8
galaxies that, together with reports of a gamma-ray burst at z ~ 8.2 (refs 10,
11), constitute the earliest objects reliably reported to date. Observations of
z ~ 7-8 galaxies suggest substantial star formation at z > 9-10. Here we use
the full two-year HUDF09 data to conduct an ultra-deep search for z ~ 10
galaxies in the heart of the reionization epoch, only 500 Myr after the Big
Bang. Not only do we find one possible z ~ 10 galaxy candidate, but we show
that, regardless of source detections, the star formation rate density is much
smaller (~10%) at this time than it is just ~200 Myr later at z ~ 8. This
demonstrates how rapid galaxy build-up was at z ~ 10, as galaxies increased in
both luminosity density and volume density from z ~ 8 to z ~ 10. The 100-200
Myr before z ~ 10 is clearly a crucial phase in the assembly of the earliest
galaxies.Comment: 41 pages, 14 figures, 2 tables, Nature, in pres
The VLA-COSMOS Perspective on the IR-Radio Relation. I. New Constraints on Selection Biases and the Non-Evolution of the IR/Radio Properties of Star Forming and AGN Galaxies at Intermediate and High Redshift
VLA 1.4 GHz (rms noise ~0.012 mJy) and MIPS 24 and 70 micron (rms noise ~0.02
and ~1.7 mJy, respectively) observations covering the 2 square degree COSMOS
field are combined with an extensive multi-wavelength data set to study the
evolution of the IR-radio relation at intermediate and high redshift. With
~4500 sources -- of which ~30% have spectroscopic redshifts -- the current
sample is significantly larger than previous ones used for the same purpose.
Both monochromatic IR/radio flux ratios (q24 & q70), as well as the ratio of
the total IR and the 1.4 GHz luminosity (qTIR) are used as indicators for the
IR/radio properties of star forming galaxies and AGN.
Using a sample jointly selected at IR and radio wavelengths in order to
reduce selection biases, we provide firm support for previous findings that the
IR-radio relation remains unchanged out to at least z~1.4. Moreover, based on
data from ~150 objects we also find that the local relation likely still holds
at 2.5<z<5. At redshift z<1.4 we observe that radio-quiet AGN populate the
locus of the IR-radio relation in similar numbers as star forming sources. In
our analysis we employ the methods of survival analysis in order to ensure a
statistically sound treatment of flux limits arising from non-detections. We
determine the observed shift in average IR/radio properties of IR- and radio-
selected populations and show that it can reconcile apparently discrepant
measurements presented in the literature. Finally, we also investigate
variations of the IR/radio ratio with IR and radio luminosity and find that it
hardly varies with IR luminosity but is a decreasing function of radio
luminosity.Comment: 52 pages, 23 figures (11 at reduced resolution). Accepted for
publication in ApJ
Gas fraction and depletion time of massive star forming galaxies at z~3.2: no change in global star formation process out to z>3
The observed evolution of the gas fraction and its associated depletion time in main sequence (MS) galaxies provides insights on how star formation proceeds over cosmic time. We report ALMA detections of the rest-frame ∼300µm continuum observed at 240 GHz for 45 massive (hlog(M⋆(M⊙))i = 10.7), normal star forming (hlog(sSFR(yr−1 ))i = −8.6), i.e. MS, galaxies at z ≈ 3.2 in the COSMOS field. From an empirical calibration between cold neutral, i.e. molecular and atomic, gas mass Mgas and monochromatic (rest-frame) infrared luminosity, the gas mass for this sample is derived. Combined with stellar mass M⋆ and star formation rate (SFR) estimates (from MagPhys fits) we obtain a median gas fraction of µgas = Mgas/M⋆ = 1.65+0.18 −0.19 and a median gas depletion time tdepl.(Gyr) = Mgas/SFR = 0.68+0.07 −0.08; correction for the location on the MS will only slightly change the values. The reported uncertainties are the 1σ error on the median. Our results are fully consistent with the expected flattening of the redshift evolution from the 2-SFM (2 star formation mode) framework that empirically prescribes the evolution assuming a universal, log-linear relation between SFR and gas mass coupled to the redshift evolution of the specific star formation rate (sSFR) of main sequence galaxies. While tdepl. shows only a mild dependence on location within the MS, a clear trend of increasing µgas across the MS is observed (as known from previous studies). Further we comment on trends within the MS and (in)consistencies with other studies
RELICS: The Reionization Lensing Cluster Survey and the Brightest High-z Galaxies
Massive foreground galaxy clusters magnify and distort the light of objects behind them, permitting a view into both the extremely distant and intrinsically faint galaxy populations. We present here the z ~ 6-8 candidate high-redshift galaxies from the Reionization Lensing Cluster Survey (RELICS), a Hubble and Spitzer Space Telescope survey of 41 massive galaxy clusters spanning an area of ≈200 arcmin². These clusters were selected to be excellent lenses, and we find similar high-redshift sample sizes and magnitude distributions as the Cluster Lensing And Supernova survey with Hubble (CLASH). We discover 257, 57, and eight candidate galaxies at z ~ 6, 7, and 8 respectively, (322 in total). The observed (lensed) magnitudes of the z ~ 6 candidates are as bright as AB mag ~23, making them among the brightest known at these redshifts, comparable with discoveries from much wider, blank-field surveys. RELICS demonstrates the efficiency of using strong gravitational lenses to produce high-redshift samples in the epoch of reionization. These brightly observed galaxies are excellent targets for follow-up study with current and future observatories, including the James Webb Space Telescope
The Build-Up of the Hubble Sequence in the COSMOS Field
We use ~8,600 >5e10 Msol COSMOS galaxies to study how the morphological mix
of massive ellipticals, bulge-dominated disks, intermediate-bulge disks,
bulge-less disks and irregular galaxies evolves from z=0.2 to z=1. The
morphological evolution depends strongly on mass. At M>3e11 Msol, no evolution
is detected in the morphological mix: ellipticals dominate since z=1, and the
Hubble sequence has quantitatively settled down by this epoch. At the 1e11 Msol
mass scale, little evolution is detected, which can be entirely explained with
major mergers. Most of the morphological evolution from z=1 to z=0.2 takes
place at masses 5e10 - 1e11 Msol, where: (i) The fraction of spirals
substantially drops and the contribution of early-types increases. This
increase is mostly produced by the growth of bulge-dominated disks, which vary
their contribution from ~10% at z=1 to >30% at z=0.2 (cf. the elliptical
fraction grows from ~15% to ~20%). Thus, at these masses, transformations from
late- to early-types result in disk-less elliptical morphologies with a
statistical frequency of only 30% - 40%. Otherwise, the processes which are
responsible for the transformations either retain or produce a non-negligible
disk component. (ii) The bulge-less disk galaxies, which contribute ~15% to the
intermediate-mass galaxy population at z=1, virtually disappear by z=0.2. The
merger rate since z=1 is too low to account for the disappearance of these
massive bulge-less disks, which most likely grow a bulge via secular evolution.Comment: 5 pages, 3 figures, submitted to ApJ
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