9,300 research outputs found
Gravitationally lensed radio emission associated with SMM J16359+6612, a multiply imaged submillimeter galaxy behind A2218
We report the detection of discrete, lensed radio emission from the multiply
imaged, z=2.516 submillimetre selected galaxy, SMM J16359+6612. All three
images are detected in deep WSRT 1.4 GHz and VLA 8.2 GHz observations, and the
radio positions are coincident with previous sub-mm SCUBA observations of this
system. This is the widest separation lens system to be detected in the radio
so far, and the first time that multiply imaged lensed radio emission has been
detected from a star forming galaxy -- all previous multiply-lensed radio
systems being associated with radio-loud AGN. Taking into account the total
magnification of ~45, the WSRT 1.4 GHz observations suggest a star formation
rate of 500 Solar mass/yr. The source has a steep radio spectrum (alpha -0.7)
and an intrinsic flux density of just 3 microJy at 8.2 GHz. Three other SCUBA
sources in the field are also detected by the WSRT, including SMMJ16359+66118,
a singly imaged (and magnified) arclet at z=1.034. Higher resolution radio
observations of SMMJ16359+6612 (and other highly magnified star forming
galaxies) provide a unique opportunity to study the general properties and
radio morphology of intrinsically faint, distant and obscured star forming
galaxies. They can also help to constrain the technical specification of next
generation radio telescopes, such as the Square Kilometre Array.Comment: 5 pages, 2 figures, to appear in A&A letter
New Modeling of the Lensing Galaxy and Cluster of Q0957+561: Implications for the Global Value of the Hubble Constant
The gravitational lens 0957+561 is modeled utilizing recent observations of
the galaxy and the cluster as well as previous VLBI radio data which have been
re-analyzed recently. The galaxy is modeled by a power-law elliptical mass
density with a small core while the cluster is modeled by a non-singular
power-law sphere as indicated by recent observations. Using all of the current
available data, the best-fit model has a reduced chi-squared of approximately 6
where the chi-squared value is dominated by a small portion of the
observational constraints used; this value of the reduced chi-squared is
similar to that of the recent FGSE best-fit model by Barkana et al. However,
the derived value of the Hubble constant is significantly different from the
value derived from the FGSE model. We find that the value of the Hubble
constant is given by H_0 = 69 +18/-12 (1-K) and 74 +18/-17 (1-K) km/s/Mpc with
and without a constraint on the cluster's mass, respectively, where K is the
convergence of the cluster at the position of the galaxy and the range for each
value is defined by Delta chi-squared = reduced chi-squared. Presently, the
best achievable fit for this system is not as good as for PG 1115+080, which
also has recently been used to constrain the Hubble constant, and the
degeneracy is large. Possibilities for improving the fit and reducing the
degeneracy are discussed.Comment: 22 pages in aaspp style including 6 tables and 5 figures, ApJ in
press (Nov. 1st issue
Values of H_0 from Models of the Gravitational Lens 0957+561
The lensed double QSO 0957+561 has a well-measured time delay and hence is
useful for a global determination of H0. Uncertainty in the mass distribution
of the lens is the largest source of uncertainty in the derived H0. We
investigate the range of \hn produced by a set of lens models intended to mimic
the full range of astrophysically plausible mass distributions, using as
constraints the numerous multiply-imaged sources which have been detected. We
obtain the first adequate fit to all the observations, but only if we include
effects from the galaxy cluster beyond a constant local magnification and
shear. Both the lens galaxy and the surrounding cluster must depart from
circular symmetry as well.
Lens models which are consistent with observations to 95% CL indicate
H0=104^{+31}_{-23}(1-\kthirty) km/s/Mpc. Previous weak lensing measurements
constrain the mean mass density within 30" of G1 to be kthirty=0.26+/-0.16 (95%
CL), implying H0=77^{+29}_{-24}km/s/Mpc (95% CL). The best-fitting models span
the range 65--80 km/s/Mpc. Further observations will shrink the confidence
interval for both the mass model and \kthirty.
The range of H0 allowed by the full gamut of our lens models is substantially
larger than that implied by limiting consideration to simple power law density
profiles. We therefore caution against use of simple isothermal or power-law
mass models in the derivation of H0 from other time-delay systems. High-S/N
imaging of multiple or extended lensed features will greatly reduce the H0
uncertainties when fitting complex models to time-delay lenses.Comment: AASTEX, 48 pages 4 figures, 2 tables. Also available at:
http://www.astro.lsa.umich.edu:80/users/philf/www/papers/list.htm
Chandra Observations of the Gravitationally Lensed System 2016+112
An observation of the gravitationally lensed system 2016+112 with the Chandra
X-ray Observatory has resolved a mystery regarding the proposed presence of a
dark matter object in the lens plane of this system. The Chandra ACIS
observation has clearly detected the lensed images of 2016+112 with positions
in good agreement with those reported in the optical and also detects 13
additional X-ray sources within a radius of 3.5 arcmin. Previous X-ray
observations in the direction of 2016+112 with the ROSAT HRI and ASCA SIS have
interpreted the X-ray data as arising from extended emission from a dark
cluster. However, the present Chandra observation can account for all the X-ray
emission as originating from the lensed images and additional point X-ray
sources in the field. Thus cluster parameters based on previous X-ray
observations are unreliable. We estimate an upper limit on the mass-to-light
ratio within a radius of 800 h_(50)^(-1) kpc of M/L_(V) < 190 h_(50)
(M/L_(V))_Sun. The lensed object is quite unusual, with reported narrow
emission lines in the optical that suggest it may be a type-2 quasar (Yamada
et. al. 1999). Our modeling of the X-ray spectrum of the lensed object implies
that the column density of an intrinsic absorber must lie between 3 and 85 x
10^22 cm^-2 (3 sigma confidence level). The 2-10 keV luminosity of the lensed
object, corrected for the lens magnification effect and using the above range
of intrinsic absorption, is 3 x 10^43 - 1.4 x 10^44 erg/s.Comment: 9 pages, includes 2 figures, Accepted for publication in ApJ
Probing the pc- and kpc-scale environment of the powerful radio galaxy Hercules A
We present the kpc-scale behaviour of the powerful extragalactic radio source
Hercules A and the behaviour of the intracluster gas in which the radio source
is situated. We have found that Hercules A exhibits a strong Laing-Garrington
effect. The X-ray observations have revealed an extended X-ray emission
elongated along the radio galaxy axis. The estimated temperature of the cluster
is kT = 2.45 keV and the central electron density is no~7.8 x 10^(-3) cm^(-3)
which reveals a hot, dense environment in which Hercules A is situated. From
the combined study of the radio and X-ray data we have estimated a central
value of 3<Bo (muG)<9. We also present the most recent results from the
analysis of the radio data on the pc-scale structure of the radio galaxy,
observed at 18 cm by the EVN-MERLIN array. A faint but compact radio source,
coincident with the optical centre of Hercules A was detected by the EVN at 18
mas resolution. The total flux density of the EVN core is 14.6 mJy. Its angular
size is 18 x 7 mas with a position angle of ~139 degrees. There is also
evidence for extended emission in the NW-SE direction, most probably from the
eastern pc-scale jet. If this is true then there is a misalignment between the
direction of the pc-eastern and the aligned kpc-scale jets of ~35 degrees.Comment: 7 pages, 2 figures, Submitted to PAS
Contaminant hydrogeology of solvents, gasoline, and salt
Guidebook for field trips in southwestern Maine: New England Intercollegiate Geological Conference, 78th annual meeting, Bates College, Lewiston, Maine, October 17, 18, and 19, 1986: Trip B-
Constraints on extragalactic transmitters via Breakthrough Listen
The Breakthrough Listen Initiative has embarked on a comprehensive SETI
survey of nearby stars in the Milky Way that is vastly superior to previous
efforts as measured by a wide range of different metrics. SETI surveys
traditionally ignore the fact that they are sensitive to many background
objects, in addition to the foreground target star. In order to better
appreciate and exploit the presence of extragalactic objects in the field of
view, the Aladin sky atlas and NED were employed to make a rudimentary census
of extragalactic objects that were serendipitously observed with the 100-m
Greenbank telescope observing at 1.1-1.9 GHz. For 469 target fields (assuming a
FWHM radial field-of-view of 4.2 arcminutes), NED identified a grand total of
143024 extragalactic objects, including various astrophysical exotica e.g. AGN
of various types, radio galaxies, interacting galaxies, and one confirmed
gravitational lens system. Several nearby galaxies, galaxy groups and galaxy
clusters are identified, permitting the parameter space probed by SETI surveys
to be significantly extended. Constraints are placed on the luminosity function
of potential extraterrestrial transmitters assuming it follows a simple power
law and limits on the prevalence of very powerful extraterrestrial transmitters
associated with these vast stellar systems are also determined. It is
demonstrated that the recent Breakthrough Listen Initiative, and indeed many
previous SETI radio surveys, place stronger limits on the prevalence of
extraterrestrial intelligence in the distant Universe than is often fully
appreciated.Comment: 9 Pages, 5 figures, accepted by MNRA
A Proof of Concept Study on Utilising a Non-invasive Microwave Analysis Technique to Characterise Silver Based Materials in Aqueous Solution
This paper reports on the feasibility of using a novel and robust microwave sensing technique to analyse and detect silver materials in an aqueous solution. Two products are tested, namely: silver chloride and silver oxide. The study mainly focused on indicating the difference between them and also any change in the size/size distribution of the sample. A microwave sensor designed previously is utilised to identify the potential of the technique to carry out the analysis. The results are presented as microwave spectrums that are the material response to microwaves. The results have shown that the technique has reasonably indicated the change in material type as well as size distribution. The results also show that these curves are distinguishable and can be related to the material and the change in its size. It is concluded that there is a potential of extending this technique to determine various other properties of silver products. The study suggests a design and development of a bespoke unit as a dedicated analysis tool and to address any anomalies arising from the current feasibility. This will have a huge industrial benefit in terms of cost reduction and time associated with the industrial analysis of silver material
String and M-theory: answering the critics
Using as a springboard a three-way debate between theoretical physicist Lee
Smolin, philosopher of science Nancy Cartwright and myself, I address in
layman's terms the issues of why we need a unified theory of the fundamental
interactions and why, in my opinion, string and M-theory currently offer the
best hope. The focus will be on responding more generally to the various
criticisms. I also describe the diverse application of string/M-theory
techniques to other branches of physics and mathematics which render the whole
enterprise worthwhile whether or not "a theory of everything" is forthcoming.Comment: Update on EPSRC. (Contribution to the Special Issue of Foundations of
Physics: "Forty Years Of String Theory: Reflecting On the Foundations",
edited by Gerard 't Hooft, Erik Verlinde, Dennis Dieks and Sebastian de Haro.
22 pages latex
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