371 research outputs found
The Dark Energy Equation of State using Alternative High-z Cosmic Tracers
We propose to use alternative cosmic tracers to measure the dark energy
equation of state and the matter content of the Universe [w(z) & Omega_m]. Our
proposed method consists of two components: (a) tracing the Hubble relation
using HII galaxies which can be detected up to very large redshifts, z~4, as an
alternative to supernovae type Ia, and (b) measuring the clustering pattern of
X-ray selected AGN at a median redshift of z~1. Each component of the method
can in itself provide interesting constraints on the cosmological parameters,
especially under our anticipation that we will reduce the corresponding random
and systematic errors significantly. However, by joining their likelihood
functions we will be able to put stringent cosmological constraints and break
the known degeneracies between the dark energy equation of state (whether it is
constant or variable) and the matter content of the universe and provide a
powerful and alternative route to measure the contribution to the global
dynamics and the equation of state of dark energy. A preliminary joint analysis
of X-ray selected AGN (based on the largest to-date XMM survey; the 2XMM) and
the currently largest SNIa sample (Hicken et al.), using as priors a flat
universe and the WMAP5 normalization of the power-spectrum, provides:
Omega_m=0.27+-0.02 and w=-0.96+-0.07. Equivalent and consistent results are
provided by the joint analysis of X-ray selected AGN clustering and the latest
Baryonic Acoustic Oscillation measures, providing: Omega_m=0.27+-0.02 and
w=-0.97+-0.04.Comment: Different versions of this paper appear in the "Dark Universe"
conference (Paris, July 2009) and in the "1st Mediterranean Conference in
Classical & Quantum Gravity" (invited
Extensions around z=2 QSOs
Based on an R-band imaging survey of 6 high redshift (z~2) and high
luminosity (M<-28mag) QSOs, we report the detection of extensions in two
radio-quiet and one radio-loud QSO. The extensions are most likely due to the
host galaxies of these QSOs, with luminosities of at least 3-7 per cent of the
QSO luminosity. The most likely values for the luminosity of the host galaxies
lie in the range $6-18 per cent of the QSO luminosity.Comment: uuencoded compressed postscript. The preprint is also available at
http://www.ast.cam.ac.uk/preprint/PrePrint.htm
Multicolour imaging of z= 2 QSO hosts
We present multicolour images of the hosts of three z=2 QSOs previously
detected in R-band by our group. The luminosities, colours and sizes of the
hosts overlap with those of actively star-forming galaxies in the nearby
Universe. Radial profiles over the outer resolved areas roughly follow de
Vaucouleur or exponential disk laws. These properties give support to the host
galaxy interpretation of the extended light around QSOs at high-redshift. The
rest-frame UV colours and upper limits derived for the rest-frame UV-optical
colours are inconsistent with the hypothesis of a scattered halo of light from
the active nucleus by a simple optically-thin scattering process produced by
dust or hot electrons. If the UV light is indeed stellar, star formation rates
of hundreds of solar masses per year are implied, an order of magnitude larger
than field galaxies at similar redshifts and above. This might indicate that
the QSO phenomenon (at least the high-luminosity one) is preferentially
acompanied by enhanced galactic activity at high-redshifts.Comment: Accepted to be published in MNRAS. 11 pages, Latex, uses mn macros,
also available at http://www.mpa-garching.mpg.de/~itzia
Thermal Emission from HII Galaxies: Discovering the Youngest Systems
We studied the radio properties of very young massive regions of star
formation in HII galaxies, with the aim of detecting episodes of recent star
formation in an early phase of evolution where the first supernovae start to
appear. Our sample consists of 31 HII galaxies, characterized by strong
Hydrogen emission lines, for which low resolution VLA 3.5cm and 6cm
observations were obtained. The radio spectral energy distribution has a range
of behaviours; 1) there are galaxies where the SED is characterized by a
synchrotron-type slope, 2) galaxies with a thermal slope, and, 3) galaxies with
possible free-free absorption at long wavelengths. The latter SEDs were found
in a few galaxies and represent a signature of heavily embedded massive star
clusters closely related to the early stages of massive star formation. Based
on the comparison of the star formation rates determined from the recombination
lines and those determined from the radio emission we find that SFR(Ha) is on
average five times higher than SFR(1.4GHz). We confirm this tendency by
comparing the ratio between the observed flux at 20 cm and the expected one,
calculated based on the Ha star formation rates, both for the galaxies in our
sample and for normal ones. This analysis shows that this ratio is a factor of
2 smaller in our galaxies than in normal ones, indicating that they fall below
the FIR/radio correlation. These results suggest that the emission of these
galaxies is dominated by a recent and massive star formation event in which the
first supernovae (SN) just started to explode. We conclude that the systematic
lack of synchrotron emission in those systems with the largest equivalent width
of Hb can only be explained if those are young starbursts of less than 3.5Myr
of age.Comment: Accepted for publication in Ap
Optical Monitoring of Quasars: I. Variability
We present an analysis of quasar variability from data collected during a
photometric monitoring of 50 objects carried out at CNPq/Laboratorio Nacional
de Astrofisica, Brazil, between March 1993 and July 1996. A distinctive feature
of this survey is its photometric accuracy, ~ 0.02 V mag, achieved through
differential photometry with CCD detectors, what allows the detection of faint
levels of variability. We find that the relative variability, delta = sigma /
L, observed in the V band is anti-correlated with both luminosity and redshift,
although we have no means of discovering the dominant relation, given the
strong coupling between luminosity and redshift for the objects in our
sample.We introduce a model for the dependence of quasar variability on
frequency that is consistent with multi-wavelength observations of the nuclear
variability of the Seyfert galaxy NGC 4151. We show that correcting the
observed variability for this effect slightly increases the significance of the
trends of variability with luminosity and redshift. Assuming that variability
depends only on the luminosity, we show that the corrected variability is
anti-correlated with luminosity and is in good agreement with predictions of a
simple Poissonian model. The energy derived for the hypothetical pulses, ~
10^50 erg, agrees well with those obtained in other studies. We also find that
the radio-loud objects in our sample tend to be more variable than the
radio-quiet ones, for all luminosities and redshifts.Comment: 17 pages, 12 figures, accepted for publication in MNRAS (uses MNRAS
style
Photometric Variability and Astrometric Stability of the Radio Continuum Nucleus in the Seyfert Galaxy NGC 5548
The NRAO VLA and VLBA were used from 1988 November to 1998 June to monitor
the radio continuum counterpart to the optical broad line region (BLR) in the
Seyfert galaxy NGC 5548. Photometric and astrometric observations were obtained
at 21 epochs. The radio nucleus appeared resolved, so comparisons were limited
to observations spanning 10-60 days and 3-4 yr, and acquired at matched
resolutions of 1210 mas = 640 pc (9 VLA observations), 500 mas = 260 pc (9 VLA
observations), or 2.3 mas = 1.2 pc (3 VLBA observations). The nucleus is
photometrically variable at 8.4 GHz by % and % between VLA
observations separated by 41 days and 4.1 yr, respectively. The 41-day changes
are milder (%) at 4.9 GHz and exhibit an inverted spectrum (, ) from 4.9 to 8.4 GHz. The nucleus
is astrometrically stable at 8.4 GHz, to an accuracy of 28 mas = 15 pc between
VLA observations separated by 4.1 yr and to an accuracy of 1.8 mas = 0.95 pc
between VLBA observations separated by 3.1 yr. Such photometric variability and
astrometric stability is consistent with a black hole being the ultimate energy
source for the BLR, but is problematic for star cluster models that treat the
BLR as a compact supernova remnant and, for NGC 5548, require a new supernova
event every 1.7 yr within an effective radius 42 mas = 22 pc. A deep
image at 8.4 GHz with resolution 660 mas = 350 pc was obtained by adding data
from quiescent VLA observations. This image shows faint bipolar lobes
straddling the radio nucleus and spanning 12 arcsec = 6.4 kpc. These
synchrotron-emitting lobes could be driven by twin jets or a bipolar wind from
the Seyfert 1 nucleus.Comment: with 9 figures, to appear in the Astrophysical Journal, 2000 March
10, volume 53
- âŠ