74 research outputs found
High-Energy Astrophysics in the 2020s and Beyond
With each passing decade, we gain new appreciation for the dynamic,
connected, and often violent nature of the Universe. This reality necessarily
places the study of high-energy processes at the very heart of modern
astrophysics. This White Paper illustrates the central role of high-energy
astrophysics to some of the most pressing astrophysical problems of our time,
the formation/evolution of galaxies, the origin of the heavy elements, star and
planet formation, the emergence of life on exoplanets, and the search for new
physics. We also highlight the new connections that are growing between
astrophysicists and plasma physicists. We end with a discussion of the
challenges that must be addressed to realize the potential of these
connections, including the need for integrated planning across physics and
astronomy programs in multiple agencies, and the need to foster the creativity
and career aspirations of individual scientists in this era of large projects.Comment: Astro2020 White Paper submissio
The multi-epoch X-ray tale of I Zwicky 1 outflows
The narrow-line Seyfert 1 galaxy I Zwicky 1 shows a unique and complex system
of ionised gas in outflow, which consists of an ultra-fast wind and a
two-component warm absorber. In the last two decades, XMM-Newton monitored the
source multiple times enabling the study of the long-term variability of the
various outflows. Plasma in photoionisation equilibrium with the ionising
source responds and varies accordingly to any change of the ionising
luminosity. However, detailed modelling of the past RGS data has shown no
correlation between the plasma ionisation state and the ionising continuum,
revealing a complex long-term variability of the multi-phase warm absorber.
Here, we present a new observation of I Zwicky 1 by XMM-Newton taken in early
2020 characterised by a lower X-ray flux state. The soft X-ray spectrum from
the RGS reveals the two components of the warm absorber with and . Comparing our results with the previous
observations, the ionisation state of the two absorbing gas components is
continuously changing, following the same unpredictable behaviour. The new
results strengthen the scenario in which the ionisation state of the warm
absorber is driven by the density of the gas rather than the ionising
luminosity. In particular, the presence of a radiation driven, inhomogeneous
clumpy outflow may explain both the variability in ionisation throughout the
years and the line-locked N V system observed in the UV band. Finally, the
EPIC-pn spectrum reveals an ultra-fast wind with an outflow velocity of and ionisation parameter of .Comment: 16 pages, 11 figures, 3 tables, accepted for publication in MNRA
Quasars with PV broad absorption in BOSS data release 9
Broad absorption lines (BALs) found in a significant fraction of quasar
spectra identify high-velocity outflows that might be present in all quasars
and could be a major factor in feedback to galaxy evolution. Understanding the
nature of these flows requires further constraints on their physical
properties, including their column densities, for which well-studied BALs, such
as CIV 1548,1551, typically provide only a lower limit because of saturation
effects. Low-abundance lines, such as PV 1118,1128, indicate large column
densities, implying outflows more powerful than measurements of CIV alone would
indicate. We search through a sample of 2694 BAL quasars from the SDSS-III/BOSS
DR9 quasar catalog for such absorption, and we identify 81 `definite' and 86
`probable' detections of PV broad absorption, yielding a firm lower limit of
3.0-6.2% for the incidence of such absorption among BAL quasars. The
PV-detected quasars tend to have stronger CIV and SiIV absorption, as well as a
higher incidence of LoBAL absorption, than the overall BAL quasar population.
Many of the PV-detected quasars have CIV troughs that do not reach zero
intensity (at velocities where PV is detected), confirming that the outflow gas
only partially covers the UV continuum source. PV appears significantly in a
composite spectrum of non-PV-detected BAL quasars, indicating that PV
absorption (and large column densities) are much more common than indicated by
our search results. Our sample of PV detections significantly increases the
number of known PV detections, providing opportunities for follow-up studies to
better understand BAL outflow energetics.Comment: 18 pages, 12 figures. All spectral plots available at
http://www.dancapellupo.com/boss-pv-bal-spectral-plots.htm
Near Infrared Spectra and Intrinsic Luminosities of Candidate Type II Quasars at 2 < z < 3.4
We present JHK near-infrared (NIR) spectroscopy of 25 candidate Type II
quasars selected from the Sloan Digital Sky Survey, using Triplespec on the
Apache Point Observatory 3.5m telescope, FIRE at the Magellan/Baade 6.5m
telescope, and GNIRS on Gemini. At redshifts of 2 < z < 3.4, our NIR spectra
probe the rest-frame optical region of these targets, which were initially
selected to have strong lines of CIV and Ly alpha, with FWHM<2000 km/s from the
SDSS pipeline. We use the [OIII]5007 line shape as a model for the narrow line
region emission, and find that \halpha\ consistently requires a broad component
with FWHMs ranging from 1000 to 7500 km/s. Interestingly, the CIV lines also
require broad bases, but with considerably narrower widths of 1000 to 4500
km/s. Estimating the extinction using the Balmer decrement and also the
relationship in lower-z quasars between rest equivalent width and luminosity in
the [OIII] line, we find typical A_V values of 0-2 mag, which naturally explain
the attenuated CIV lines relative to Halpha. We propose that our targets are
moderately obscured quasars. We also describe one unusual object with three
distinct velocity peaks in its [OIII] spectrum.Comment: Accepted for publication in ApJ, 18 pages, 14 figure
The z=5 Quasar Luminosity Function from SDSS Stripe 82
We present a measurement of the Type I quasar luminosity function at z=5
using a large sample of spectroscopically confirmed quasars selected from
optical imaging data. We measure the bright end (M_1450<-26) with Sloan Digital
Sky Survey (SDSS) data covering ~6000 deg^2, then extend to lower luminosities
(M_1450<-24) with newly discovered, faint z~5 quasars selected from 235 deg^2
of deep, coadded imaging in the SDSS Stripe 82 region (the celestial equator in
the Southern Galactic Cap). The faint sample includes 14 quasars with spectra
obtained as ancillary science targets in the SDSS-III Baryon Oscillation
Spectroscopic Survey (BOSS), and 59 quasars observed at the MMT and Magellan
telescopes. We construct a well-defined sample of 4.7<z<5.1 quasars that is
highly complete, with 73 spectroscopic identifications out of 92 candidates.
Our color selection method is also highly efficient: of the 73 spectra
obtained, 71 are high redshift quasars. These observations reach below the
break in the luminosity function (M_1450* ~ -27). The bright end slope is steep
(beta <~ -4), with a constraint of beta < -3.1 at 95% confidence. The break
luminosity appears to evolve strongly at high redshift, providing an
explanation for the flattening of the bright end slope reported previously. We
find a factor of ~2 greater decrease in the number density of luminous quasars
(M_1450<-26) from z=5 to z=6 than from z=4 to z=5, suggesting a more rapid
decline in quasar activity at high redshift than found in previous surveys. Our
model for the quasar luminosity function predicts that quasars generate ~30% of
the ionizing photons required to keep the universe ionized at z=5.Comment: 29 pages, 22 figures, ApJ accepted (updated to published version
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