64 research outputs found
Can Cosmological Simulations Reproduce the Spectroscopically Confirmed Galaxies Seen at ?
Recent photometric detections of extreme redshift galaxies from the
JWST have been shown to be in strong tension with existing simulation models
for galaxy formation, and in the most acute case, in tension with
itself. These results, however, all rest on the confirmation of these distances
by spectroscopy. Recently, the JADES survey has detected the most distant
galaxies with spectroscopically confirmed redshifts, with four galaxies found
with redshifts between and . In this paper, we compare
simulation predictions from four large cosmological volumes and two zoom-in
protoclusters with the JADES observations to determine whether these
spectroscopically confirmed galaxy detections are in tension with existing
models for galaxy formation, or with more broadly. We find that
existing models for cosmological galaxy formation can generally reproduce the
observations for JADES, in terms of galaxy stellar masses, star formation
rates, and the number density of galaxies at .Comment: ApJL submitted, comments welcom
Reionization with galaxies and active galactic nuclei
In this work we investigate the properties of the sources that reionized the intergalactic medium (IGM) in the high-redshift Universe. Using a semi-Analytical model aimed at reproducing galaxies and black holes in the first âŒ1.5 Gyr of the Universe, we revisit the relative role of star formation and black hole accretion in producing ionizing photons that can escape into the IGM. Both star formation and black hole accretion are regulated by supernova feedback, resulting in black hole accretion being stunted in low-mass haloes. We explore a wide range of combinations for the escape fraction of ionizing photons (redshift-dependent, constant, and scaling with stellar mass) from both star formation () and AGN () to find: (i) the ionizing budget is dominated by stellar radiation from low stellar mass () galaxies at z > 6 with the AGN contribution (driven by black holes in galaxies) dominating at lower redshifts; (ii) AGN only contribute to the cumulative ionizing emissivity by z = 4 for the models that match the observed reionization constraints; (iii) if the stellar mass dependence of is shallower than , at z < 7 a transition stellar mass exists above which AGN dominate the escaping ionizing photon production rate; (iv) the transition stellar mass decreases with decreasing redshift. While AGN dominate the escaping emissivity above the knee of the stellar mass function at z âŒ6.8, they take-over at stellar masses that are a tenth of the knee mass by z = 4
Population statistics of intermediate-mass black holes in dwarf galaxies using the newhorizon simulation
While it is well established that supermassive black holes (SMBHs) coevolve with their host galaxy, it is currently less clear how lower-mass black holes, so-called intermediate-mass black holes (IMBHs), evolve within their dwarf galaxy hosts. In this paper, we present results on the evolution of a large sample of IMBHs from the NEWHORIZON zoom volume, which has a radius of 10 comoving Mpc. We show that occupation fractions of IMBHs in dwarf galaxies are at least 50 per cent for galaxies with stellar masses down to 106 Mâ, but BH growth is very limited in dwarf galaxies. In NEWHORIZON, IMBHs growth is somewhat more efficient at high redshift z = 3 but in general, IMBHs do not grow significantly until their host galaxy leaves the dwarf regime. As a result, NEWHORIZON underpredicts observed AGN luminosity function and AGN fractions. We show that the difficulties of IMBHs to remain attached to the centres of their host galaxies plays an important role in limiting their mass growth, and that this dynamic evolution away from galactic centres becomes stronger at lower redshift
Multimessenger study of merging massive black holes in the Obelisk simulation: gravitational waves, electromagnetic counterparts, and their link to galaxy and black hole populations
Massive black hole (BH) mergers are predicted to be powerful sources of
low-frequency gravitational waves (GWs). Coupling the detection of GWs with
electromagnetic (EM) detection can provide key information about merging BHs
and their environments. We study the high-resolution cosmological
radiation-hydrodynamics simulation Obelisk, run to redshift , to assess
the GW and EM detectability of high-redshift BH mergers, modelling spectral
energy distribution and obscuration. For EM detectability we further consider
sub-grid dynamical delays in postprocessing. We find that most of the merger
events can be detected by LISA, except for high-mass mergers with very unequal
mass ratios. Intrinsic binary parameters are accurately measured, but the sky
localisation is poor generally. Only of these high-redshift sources
have sky localisation better than . Merging BHs are hard to
detect in the restframe UV since they are fainter than the host galaxies, which
at high are star-forming. A significant fraction, , of BH mergers
instead outshines the galaxy in X-rays, and about are sufficiently
bright to be detected with sensitive X-ray instruments. If mergers induce an
Eddington-limited brightening, up to of sources can become observable.
The transient flux change originating from such a brightening is often large,
allowing of mergers to be detected as EM counterparts. A fraction
of mergers is also detectable at radio frequencies. Observable merging
BHs tend to have higher accretion rates and masses and are overmassive at fixed
galaxy mass with respect to the full population. Most EM-observable mergers can
also be GW-detected with LISA, but their sky localisation is generally poorer.
This has to be considered when using EM counterparts to obtain information
about the properties of merging BHs and their environment.Comment: 17 pages, 11 figures, submitted to A&
Population statistics of intermediate mass black holes in dwarf galaxies using the NewHorizon simulation
While it is well established that supermassive black holes (SMBHs) co-evolve
with their host galaxy, it is currently less clear how lower mass black holes,
so-called intermediate mass black holes (IMBHs), evolve within their dwarf
galaxy hosts. In this paper, we present results on the evolution of a large
sample of IMBHs from the NewHorizon simulation. We show that occupation
fractions of IMBHs in dwarf galaxies are at least 50 percent for galaxies with
stellar masses down to 1E6 Msun, but BH growth is very limited in dwarf
galaxies. In NewHorizon, IMBH growth is somewhat more efficient at high
redshift z = 3 but in general IMBH do not grow significantly until their host
galaxy leaves the dwarf regime. As a result, NewHorizon under-predicts observed
AGN luminosity function and AGN fractions. We show that the difficulties of
IMBH to remain attached to the centres of their host galaxies plays an
important role in limiting their mass growth, and that this dynamic evolution
away from galactic centres becomes stronger at lower redshift.Comment: 15 pages, submitted to MNRA
Gas Accretion and Giant Lyman-alpha Nebulae
Several decades of observations and discoveries have shown that high-redshift
AGN and massive galaxies are often surrounded by giant Lyman-alpha nebulae
extending in some cases up to 500 kpc in size. In this review, I discuss the
properties of the such nebulae discovered at z>2 and their connection with gas
flows in and around the galaxies and their halos. In particular, I show how
current observations are used to constrain the physical properties and origin
of the emitting gas in terms of the Lyman-alpha photon production processes and
kinematical signatures. These studies suggest that recombination radiation is
the most viable scenario to explain the observed Lyman-alpha luminosities and
Surface Brightness for the large majority of the nebulae and imply that a
significant amount of dense, ionized and cold clumps should be present within
and around the halos of massive galaxies. Spectroscopic studies suggest that,
among the giant Lyman-alpha nebulae, the one associated with radio-loud AGN
should have kinematics dominated by strong, ionized outflows within at least
the inner 30-50 kpc. Radio-quiet nebulae instead present more quiescent
kinematics compatible with stationary situation and, in some cases, suggestive
of rotating structures. However, definitive evidences for accretion onto
galaxies of the gas associated with the giant Lyman-alpha emission are not
unambiguously detected yet. Deep surveys currently ongoing using other bright,
non-resonant lines such as Hydrogen H-alpha and HeII1640 will be crucial to
search for clearer signatures of cosmological gas accretion onto galaxies and
AGN.Comment: Invited review to appear in Gas Accretion onto Galaxies, Astrophysics
and Space Science Library, eds. A. J. Fox & R. Dave', to be published by
Springe
A quasar-galaxy merger at z ~ 6.2: Black hole mass and quasar properties from the NIRSpec spectrum
We present JWST/NIRSpec integral field data of the quasar PJ308-21 at z = 6.2342. As shown by previous ALMA and HST imaging, the quasar has two companion sources, interacting with the quasar host galaxy. The high-resolution G395H/290LP NIRSpec spectrum covers the 2.87 â 5.27 ÎŒm wavelength range and shows the rest-frame optical emission of the quasar with exquisite quality (signal-to-noise ratio âŒ100 â 400 per spectral element). Based on the HÎČ line from the broad line region, we obtain an estimate of the black hole mass MBH, HÎČ âŒ 2.7 Ă 109 Mâ. This value is within a factor âČ1.5 of the Hα-based black hole mass from the same spectrum (MBH, Hα ⌠1.93 Ă 109 Mâ) and is consistent with a previous estimate relying on the Mg IIλ2799 line (MBH, MgII ⌠2.65 Ă 109 Mâ). All these MBH estimates are within the âŒ0.5 dex intrinsic scatter of the adopted mass calibrations. The high Eddington ratio of PJ308-21 λEdd, HÎČ âŒ 0.67 (λEdd, Hα ⌠0.96) is in line with the overall quasar population at z âł 6. The relative strengths of the [O III], Fe II, and HÎČ lines are consistent with the empirical âEigenvector 1â correlations as observed for low redshift quasars. We find evidence for blueshifted [O III] λ5007 emission with a velocity offset Îv[O III] = â1922 ± 39 km sâ1 from the systemic velocity and a full width at half maximum (FWHM) FWHM([O III]) = 2776â74+75 km sâ1. This may be the signature of outflowing gas from the nuclear region, despite the true values of Îv[O III] and FWHM([O III]) likely being more uncertain due to the blending with HÎČ and Fe II lines. Our study demonstrates the unique capabilities of NIRSpec in capturing quasar spectra at cosmic dawn and studying their properties in unprecedented detail
The Low-Redshift Lyman Continuum Survey. Unveiling the ISM properties of low- Lyman continuum emitters
Combining 66 ultraviolet (UV) spectra and ancillary data from the
Low-Redshift Lyman Continuum Survey (LzLCS) and 23 LyC observations by earlier
studies, we form a statistical sample of star-forming galaxies at
to study the role of the cold interstellar medium (ISM) gas in the leakage of
ionizing radiation. We first constrain the massive star content (ages and
metallicities) and UV attenuation, by fitting the stellar continuum with a
combination of simple stellar population models. The models, together with
accurate LyC flux measurements, allow to determine the absolute LyC photon
escape fraction for each galaxy (). We measure the
equivalent widths and residual fluxes of multiple HI and low-ionization state
(LIS) lines, and the geometrical covering fraction adopting the picket-fence
model. The spans a wide range, with a median (0.16,
0.84 quantiles) of 0.04 (0.02, 0.20), and 50 out of the 89 galaxies detected in
the LyC. The HI and LIS line equivalent widths scale with the UV luminosity and
attenuation, and inversely with the residual flux of the lines. The HI and LIS
residual fluxes are correlated, indicating that the neutral gas is spatially
traced by the LIS transitions. We find the observed trends of the absorption
lines and the UV attenuation are primarily driven by the covering fraction. The
non-uniform gas coverage demonstrates that LyC photons escape through
low-column density channels in the ISM. The equivalent widths and residual
fluxes of the UV lines strongly correlate with : strong
LyC leakers show weak absorption lines, low UV attenuation, and large
Ly equivalent widths. We finally show that simultaneous UV absorption
line and dust attenuation measurements can predict, on average, the escape
fraction of galaxies and the method can be applied to galaxies across a wide
redshift range.Comment: 30 pages, 16 figures, 3 tables; accepted for publication in Astronomy
and Astrophysics on December 16, 2021. Tables A1 to A4 are part of the LzLCS
science products and will be publicly available in a dedicated websit
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