85 research outputs found
A 1200-micron MAMBO survey of ELAISN2 and the Lockman Hole - I. Maps, sources and number counts
The definitive version is available at www.blackwell-synergy.com '.--Copyright Blackwell Publishing. DOI : 10.1111/j.1365-2966.2004.08235.xWe present a deep, new 1200μm survey of the ELAISN2 and Lockman Hole fields using the Max Planck Millimeter Bolometer array (MAMBO). The areas surveyed are 160 arcmin2 in ELAISN2 and 197 arcmin2 in the Lockman Hole, covering the entire SCUBA ‘8mJy Survey’. In total, 27 (44) sources have been detected at a significance 4.0 ( 3.5 ). The primary goals of the survey were to investigate the reliability of (sub)millimetre galaxy (SMG) samples, to analyse SMGs using flux ratios sensitive to redshift at z > 3, and to search for ‘SCUBA drop-outs’, i.e. galaxies at z >> 3. We present the 1200μm number counts and find evidence of a fall at bright flux levels. Employing parametric models for the evolution of the local 60μm IRAS luminosity function (LF), we are able to account simultaneously for the 1200 and 850μm counts, suggesting that the MAMBO and SCUBA sources trace the same underlying population of high-redshift, dust-enshrouded galaxies. From a nearest-neighbour clustering analysis we find tentative evidence that themost significantMAMBO sources come in pairs, typically separated by 23′′. Our MAMBO observations unambiguously confirm around half of the SCUBA sources. In a robust sub-sample of 13 SMGs detected by both MAMBO and SCUBA at a significance 3.5 , only one has no radio counterpart. Furthermore, the distribution of 850/1200μmflux density ratios for this sub-sample is consistent with the spectroscopic redshift distribution of radio-detected SMGs (Chapman et al. 2003). Finally, we have searched for evidence of a high-redshift tail of SMGs amongst the 18 MAMBO sources which are not detected by SCUBA. While we cannot rule out that some of them are SCUBA drop-outs at z >> 3, their overall 850-to-1200μm flux distribution is statistically indistinguishable from that of the 13 SMGS which were robustly identified by both MAMBO and SCUBA.Peer reviewe
Numerical studies on the structure of the cosmic ray electron halo in starburst galaxies
The structure of the cosmic ray electron halo of a starburst galaxy depends
strongly on the nature of galactic wind and the configuration of the magnetic
field. We have investigated these dependencies by solving numerically the
propagation of electrons originating in starburst galaxies, most likely in
supernova remnants. The calculations are made for several models for the
galactic winds and for the configuration of the magnetic fields for comparison
with observations. Our simulation of a quasi-radio halo reproduces both the
extended structure of ~ 9 kpc and the subtle hollow structure near the polar
region of the radio halo that are observed in the starburst galaxy NGC 253.
These findings suggest the existence of strong galactic wind in NGC 253.Comment: 4 pages, 6 figures, to appear in Proceeding of the conference "The
multi messenger approach to high energy gamma ray sources", Barcelona, July
200
Radio Source Heating in the ICM: The Example of Cygnus A
One of the most promising solutions for the cooling flow problem involves
energy injection from the central AGN. However it is still not clear how
collimated jets can heat the ICM at large scale, and very little is known
concerning the effect of radio lobe expansion as they enter into pressure
equilibrium with the surrounding cluster gas. Cygnus A is one of the best
examples of a nearby powerful radio galaxy for which the synchrotron emitting
plasma and thermal emitting intra-cluster medium can be mapped in fine detail,
and previous observations have inferred possible shock structure at the
location of the cocoon. We use new XMM-Newton observations of Cygnus A, in
combination with deep Chandra observations, to measure the temperature of the
intra-cluster medium around the expanding radio cavities. We investigate how
inflation of the cavities may relate to shock heating of the intra-cluster gas,
and whether such a mechanism is sufficient to provide enough energy to offset
cooling to the extent observed.Comment: To appear in the Proceedings of "Heating vs. Cooling in Galaxies and
Clusters of Galaxies", August 2006, Garching (Germany), Eds. H. Boehringer,
G.W. Pratt, A. Finoguenov, P. Schuecker, Springer-Verlag series "ESO
Astrophysics Symposia", p.101, in press. 8 pages, 3 multiple figure
Observational constraints on Cosmic Reionization
Recent observations have set the first constraints on the epoch of
reionization (EoR), corresponding to the formation epoch of the first luminous
objects. Studies of Gunn-Peterson (GP) absorption, and related phenomena,
suggest a qualitative change in the state of the intergalactic medium (IGM) at
, indicating a rapid increase in the neutral fraction of the IGM,
from , perhaps up to
0.1, at . Conversely, transmission spikes in the GP trough, and the
evolution of the \lya galaxy luminosity function indicate at
, while the large scale polarization of the cosmic microwave
background (CMB) implies a significant ionization fraction extending to higher
redshifts, . The results suggest that reionization is less an
event than a process, with the process beginning as early as , and
with the 'percolation', or 'overlap' phase ending at . The data are
consistent with low luminosity star forming galaxies as being the dominant
sources of reionizing photons. Low frequency radio telescopes currently under
construction should be able to make the first direct measurements of HI 21cm
emission from the neutral IGM during the EoR, and upcoming measurements of
secondary CMB temperature anisotropy will provide fine details of the dynamics
of the reionized IGM.Comment: to appear in ARAA 2006, vol 44, page 415-462; latex. 84 pages. 15 fi
Integrated Filterbank for DESHIMA: A Submillimeter Imaging Spectrograph Based on Superconducting Resonators
An integrated filterbank (IFB) in combination with microwave kinetic
inductance detectors (MKIDs), both based on superconducting resonators, could
be used to make broadband submillimeter imaging spectrographs that are compact
and flexible. In order to investigate the possibility of adopting an IFB
configuration for DESHIMA (Delft SRON High-redshift Mapper), we study the basic
properties of a coplanar-waveguide-based IFB using electromagnetic simulation.
We show that a coupling efficiency greater than 1/2 can be achieved if
transmission losses are negligible. We arrive at a practical design for a 9
pixel x 920 color 3 dimensional imaging device that fits on a 4 inch wafer,
which instantaneously covers multiple submillimeter telluric windows with a
dispersion of f/df = 1000.Comment: 6 pages, 4 figures, submitted to LTD-14 / Journal of Low Temperature
Physic
AGN effect on cooling flow dynamics
We analyzed the feedback of AGN jets on cooling flow clusters using
three-dimensional AMR hydrodynamic simulations. We studied the interaction of
the jet with the intracluster medium and creation of low X-ray emission
cavities (Bubbles) in cluster plasma. The distribution of energy input by the
jet into the system was quantified in its different forms, i.e. internal,
kinetic and potential. We find that the energy associated with the bubbles, (pV
+ gamma pV/(gamma-1)), accounts for less than 10 percent of the jet energy.Comment: "Accepted for publication in Astrophysics & Space Science
Demonstrating the Feasibility of Line Intensity Mapping Using Mock Data of Galaxy Clustering from Simulations
Visbal & Loeb (2010) have shown that it is possible to measure the clustering
of galaxies by cross correlating the cumulative emission from two different
spectral lines which originate at the same redshift. Through this cross
correlation, one can study galaxies which are too faint to be individually
resolved. This technique, known as intensity mapping, is a promising probe of
the global properties of high redshift galaxies. Here, we test the feasibility
of such measurements with synthetic data generated from cosmological dark
matter simulations. We use a simple prescription for associating galaxies with
dark matter halos and create a realization of emitted radiation as a function
of angular position and wavelength over a patch of the sky. This is then used
to create synthetic data for two different hypothetical instruments, one aboard
the Space Infrared Telescope for Cosmology and Astrophysics (SPICA) and another
consisting of a pair of ground based radio telescopes designed to measure the
CO(1-0) and CO(2-1) emission lines. We find that the line cross power spectrum
can be measured accurately from the synthetic data with errors consistent with
the analytical prediction of Visbal & Loeb (2010). Removal of astronomical
backgrounds and masking bright line emission from foreground contaminating
galaxies do not prevent accurate cross power spectrum measurements.Comment: 12 pages, 6 figures, Submitted to JCA
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