54 research outputs found
Figuring Out Gas & Galaxies In Enzo (FOGGIE) V: The Virial Temperature Does Not Describe Gas in a Virialized Galaxy Halo
The classical definition of the virial temperature of a galaxy halo excludes
a fundamental contribution to the energy partition of the halo: the kinetic
energy of non-thermal gas motions. Using simulations of low-redshift, galaxies from the FOGGIE project (Figuring Out Gas & Galaxies In Enzo)
that are optimized to resolve low-density gas, we show that the kinetic energy
of non-thermal motions is roughly equal to the energy of thermal motions. The
simulated FOGGIE halos have lower bulk temperatures than
expected from a classical virial equilibrium, owing to significant non-thermal
kinetic energy that is formally excluded from the definition of
. We derive a modified virial temperature explicitly including
non-thermal gas motions that provides a more accurate description of gas
temperatures for simulated halos in virial equilibrium. Strong bursts of
stellar feedback drive the simulated FOGGIE halos out of virial equilibrium,
but the halo gas cannot be accurately described by the standard virial
temperature even when in virial equilibrium. Compared to the standard virial
temperature, the cooler modified virial temperature implies other effects on
halo gas: (i) the thermal gas pressure is lower, (ii) radiative cooling is more
efficient, (iii) O VI absorbing gas that traces the virial temperature may be
prevalent in halos of a higher mass than expected, (iv) gas mass estimates from
X-ray surface brightness profiles may be incorrect, and (v) turbulent motions
make an important contribution to the energy balance of a galaxy halo.Comment: 30 pages, 14 figures, accepted to Ap
Figuring Out Gas & Galaxies in Enzo (FOGGIE). III. The Mocky Way:Investigating Biases in Observing the Milky Way's Circumgalactic Medium
The circumgalactic medium (CGM) of the Milky Way is mostly obscured by nearby
gas in position-velocity space because we reside inside the Galaxy. Substantial
biases exist in most studies on the Milky Way's CGM that focus on
easier-to-detect high-velocity gas. With mock observations on a Milky-Way
analog from the FOGGIE simulation, we investigate four observational biases
related to the Milky Way's CGM. First, QSO absorption-line studies probe a
limited amount of the CGM mass: only 35% of the mass is at high Galactic
latitudes degrees, of which only half is moving at km s. Second, the inflow rate () of the cold
gas observable in HI 21cm is reduced by a factor of as we switch from
the local standard of rest to the galaxy's rest frame; meanwhile of
the cool and warm gas does not change significantly. Third, OVI and NV are
promising ions to probe the Milky Way's outer CGM (15 kpc), but CIV
may be less sensitive. Lastly, the scatter in ion column density is a factor of
2 higher if the CGM is observed from inside-out than from external views
because of the gas radial density profile. Our work highlights that
observations of the Milky Way's CGM, especially those using HI 21cm and QSO
absorption lines, are highly biased. We demonstrate that these biases can be
quantified and calibrated through synthetic observations with simulated
Milky-Way analogs.Comment: ApJ in pres
Figuring Out Gas & Galaxies In Enzo (FOGGIE) VIII: Complex and Stochastic Metallicity Gradients at z > 2
Gas-phase metallicity gradients are a crucial element in understanding the
chemical evolution of galaxies. We use the FOGGIE simulations to study the
metallicity gradients () of six Milky Way-like galaxies throughout
their evolution. FOGGIE galaxies generally exhibit steep negative gradients for
most of their history, with only a few short-lived instances reaching positive
slopes that appear to arise mainly from interactions with other galaxies.
FOGGIE concurs with other simulation results but disagrees with the robust
observational finding that flat and positive gradients are common at . By
tracking the metallicity gradient at a rapid cadence of simulation outputs
(--10 Myr), we find that theoretical gradients are highly stochastic:
the FOGGIE galaxies spend \% of their time far away from a smoothed
trajectory inferred from analytic models or other, less high-cadence
simulations. This rapid variation makes instantaneous gradients from
observations more difficult to interpret in terms of physical processes.
Because of these geometric and stochastic complications, we explore
non-parametric methods of quantifying the evolving metallicity distribution at
. We investigate how efficiently non-parametric measures of the 2-D
metallicity distribution respond to metal production and mixing. Our results
suggest that new methods of quantifying and interpreting gas-phase metallicity
will be needed to relate trends in upcoming high- {\it JWST} observations
with the underlying physics of gas accretion, expulsion, and recycling in early
galaxies.Comment: Submitted to Ap
Figuring Out Gas & Galaxies In Enzo (FOGGIE). IV. The Stochasticity of Ram Pressure Stripping in Galactic Halos
We study ram pressure stripping in simulated Milky Way-like halos at z>=2
from the Figuring Out Gas & Galaxies In Enzo (FOGGIE) project. These
simulations reach exquisite resolution in their circumgalactic medium (CGM) gas
owing to FOGGIE's novel refinement scheme. The CGM of each halo spans a wide
dynamic range in density and velocity over its volume---roughly 6 dex and 1000
km/s, respectively---translating into a 5 dex range in ram pressure imparted to
interacting satellites. The ram pressure profiles of the simulated CGM are
highly stochastic, owing to kpc-scale variations of the density and velocity
fields of the CGM gas. As a result, the efficacy of ram pressure stripping
depends strongly on the specific path a satellite takes through the CGM. The
ram-pressure history of a single satellite is generally unpredictable and not
well correlated with its approach vector with respect to the host galaxy. The
cumulative impact of ram pressure on the simulated satellites is dominated by
only a few short strong impulses---on average, 90% of the total surface
momentum gained through ram pressure is imparted in 20% or less of the total
orbital time. These results reveal an erratic mode of ram pressure stripping in
Milky-Way like halos at high redshift---one that is not captured by a smooth
spherically-averaged model of the circumgalactic medium.Comment: 18 pages, 10 figures. Submitted to Ap
Ionized Gas Extended Over 40 kpc in an Odd Radio Circle Host Galaxy
A new class of extragalactic astronomical sources discovered in 2021, named
Odd Radio Circles (ORCs, Norris et al. 2021), are large rings of faint, diffuse
radio continuum emission spanning ~1 arcminute on the sky. Galaxies at the
centers of several ORCs have photometric redshifts of z~0.3-0.6, implying
physical scales of several 100 kiloparsecs in diameter for the radio emission,
the origin of which is unknown. Here we report spectroscopic data on an ORC
including strong [OII] emission tracing ionized gas in the central galaxy of
ORC4 at z=0.4512. The physical extent of the [OII] emission is ~40 kpc in
diameter, larger than expected for a typical early-type galaxy (Pandya et al,
2017) but an order of magnitude smaller than the large-scale radio continuum
emission. We detect a ~200 km/s velocity gradient across the [OII] nebula, as
well as a high velocity dispersion of ~180 km/s. The [OII] equivalent width
(EW, ~50 Ang) is extremely high for a quiescent galaxy. The morphology,
kinematics, and strength of the [OII] emission are consistent with the infall
of shock ionized gas near the galaxy, following a larger-scale, outward moving
shock driven by a galactic wind. Both the extended optical and radio emission,
while observed on very different scales, may therefore result from the same
dramatic event.Comment: 7 figures, accepted to Natur
Reverberation Mapping of Optical Emission Lines in Five Active Galaxies
We present the first results from an optical reverberation mapping campaign executed in 2014 targeting the active galactic nuclei (AGNs) MCG+08-11-011, NGC 2617, NGC 4051, 3C 382, and Mrk 374. Our targets have diverse and interesting observational properties, including a changing look AGN and a broad-line radio galaxy. Based on continuum-Hβ lags, we measure black hole masses for all five targets. We also obtain Hγ and He ii λ4686 lags for all objects except 3C 382. The He ii λ4686 lags indicate radial stratification of the BLR, and the masses derived from different emission lines are in general agreement. The relative responsivities of these lines are also in qualitative agreement with photoionization models. These spectra have extremely high signal-to-noise ratios (100-300 per pixel) and there are excellent prospects for obtaining velocity-resolved reverberation signatures
Reverberation mapping of optical emission lines in five active galaxies
For a video summarizing the main results, see https://www.youtube.com/watch?v=KaC-jPsIY0QWe present the first results from an optical reverberation mapping campaign executed in 2014 targeting the active galactic nuclei (AGNs) MCG+08-11-011, NGC 2617, NGC 4051, 3C 382, and Mrk 374. Our targets have diverse and interesting observational properties, including a "changing look" AGN and a broad-line radio galaxy. Based on continuum-Hβ lags, we measure black hole masses for all five targets. We also obtain Hγ and He ii λ4686 lags for all objects except 3C 382. The He ii λ4686 lags indicate radial stratification of the BLR, and the masses derived from different emission lines are in general agreement. The relative responsivities of these lines are also in qualitative agreement with photoionization models. These spectra have extremely high signal-to-noise ratios (100–300 per pixel) and there are excellent prospects for obtaining velocity-resolved reverberation signatures.Publisher PDFPeer reviewe
Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548
We present the results of an optical spectroscopic monitoring program targeting NGC 5548 as part of a larger multiwavelength reverberation mapping campaign. The campaign spanned 6 months and achieved an almost daily cadence with observations from five ground-based telescopes. The Hβ and He ii λ4686 broad emission-line light curves lag that of the 5100 +-optical continuum by 4.17+0.36-0.36 and 0.79+0.35-0.34 days, respectively. The Hβ lag relative to the 1158 ultraviolet continuum light curve measured by the Hubble Space Telescope is ∼50% longer than that measured against the optical continuum, and the lag difference is consistent with the observed lag between the optical and ultraviolet continua. This suggests that the characteristic radius of the broad-line region is ∼50% larger than the value inferred from optical data alone. We also measured velocity-resolved emission-line lags for Hβ and found a complex velocity-lag structure with shorter lags in the line wings, indicative of a broad-line region dominated by Keplerian motion. The responses of both the Hβ and He ii emission lines to the driving continuum changed significantly halfway through the campaign, a phenomenon also observed for C iv, Lyα, He ii(+O iii]), and Si iv(+O iv]) during the same monitoring period. Finally, given the optical luminosity of NGC 5548 during our campaign, the measured Hβ lag is a factor of five shorter than the expected value implied by the R BLR-L AGN relation based on the past behavior of NGC 5548
Space Telescope and Optical Reverberation Mapping Project. XII. broad-line region modeling of NGC 5548.
We present geometric and dynamical modeling of the broad line region (BLR) for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The data set includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the Hβ, C iv, and Lyα broad emission lines. We find an extended disk-like Hβ BLR with a mixture of near-circular and outflowing gas trajectories, while the C iv and Lyα BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with C iv and Lyα emission arising at smaller radii than the Hβ emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of . We examine the effect of using the V band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV–optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that the V band is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the Hβ results to similar models of data obtained in 2008 when the active galactic nucleus was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remained unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole
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