703 research outputs found
The WiFeS S7 AGN survey: Current status and recent results on NGC 6300
The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) is a
targeted survey probing the narrow-line regions (NLRs) of a representative
sample of ~140 nearby (z<0.02) Seyfert galaxies by means of optical integral
field spectroscopy. The survey is based on a homogeneous data set observed
using the Wide Field Spectrograph WiFeS. The data provide a 25x38 arcsec
field-of-view around the galaxy centre at typically ~1.5 arcsec spatial
resolution and cover a wavelength range between ~3400 - 7100 at spectral
resolutions of ~100 km s and ~50 km s in the blue and red parts,
respectively. The survey is primarily designed to study gas excitation and star
formation around AGN, with a special focus on the shape of the AGN ionising
continuum, the interaction between radio jets and the NLR gas, and the nature
of nuclear LINER emission. We provide an overview of the current status of
S7-based results and present new results for NGC 6300.Comment: 5 pages, 1 figure, Refereed Proceeding of the "The Universe of
Digital Sky Surveys" conference held at the INAF - Observatory of
Capodimonte, Naples, on 25th-28th november 2014, to be published on
Astrophysics and Space Science Proceedings, edited by Longo, Napolitano,
Marconi, Paolillo, Iodic
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Dual axis operation of a micromachined rate gyroscope
Since micromachining technology has raised the prospect of fabricating high performance sensors without the associated high cost and large size, many researchers have investigated micromachined rate gyroscopes. The vast majority of research has focused on single input axis rate gyroscopes, but this paper presents work on a dual input axis micromachined rate gyroscope. The key to successful simultaneous dual axis operation is the quad symmetry of the circular oscillating rotor design. Untuned gyroscopes with mismatched modes yielded random walk as low as 10{degrees}/{radical}hour with cross sensitivity ranging from 6% to 16%. Mode frequency matching via electrostatic tuning allowed performance better than 2{degrees}/{radical}hour, but at the expense of excessive cross sensitivity
Morphology and Size Differences between Local & High Redshift Luminous Infrared Galaxies
We show that the star-forming regions in high-redshift luminous and
ultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimeter galaxies
(SMGs) have similar physical scales to those in local normal star-forming
galaxies. To first order, their higher infrared (IR) luminosities result from
higher luminosity surface density. We also find a good correlation between the
IR luminosity and IR luminosity surface density in starburst galaxies across
over five orders of magnitude of IR luminosity from local normal galaxies to z
~ 2 SMGs. The intensely star-forming regions of local ULIRGs are significantly
smaller than those in their high-redshift counterparts and hence diverge
significantly from this correlation, indicating that the ULIRGs found locally
are a different population from the high-redshift ULIRGs and SMGs. Based on
this relationship, we suggest that luminosity surface density should serve as a
more accurate indicator for the IR emitting environment, and hence the
observable properties, of star-forming galaxies than their IR luminosity. We
demonstrate this approach by showing that ULIRGs at z ~ 1 and a lensed galaxy
at z ~ 2.5 exhibit aromatic features agreeing with local LIRGs that are an
order of magnitude less luminous, but have similar IR luminosity surface
density. A consequence of this relationship is that the aromatic emission
strength in star-forming galaxies will appear to increase at z > 1 for a given
IR luminosity compared to their local counterparts.Comment: Accepted for publication in The Astrophysical Journal; 13 pages, 7
figures; Online materials available at
http://inthanon.as.arizona.edu/~wiphu/Rujopakarn_2010
Interaction between vortices in models with two order parameters
The interaction energy and force between widely separated strings is analyzed
in a field theory having applications to superconducting cosmic strings, the
SO(5) model of high-temperature superconductivity, and solitons in nonlinear
optics. The field theory has two order parameters, one of which is broken in
the vacuum (giving rise to strings), the other of which is unbroken in the
vacuum but which could nonetheless be broken in the core of the string. If this
does occur, there is an effect on the energetics of widely separated strings.
This effect is important if the length scale of this second order parameter is
longer than that of the other fields in the problem.Comment: 11 pages, 3 figures. Minor changes in the text. Accepted for
publication in Phys. Rev.
A Survey of Atomic Carbon [C I] in High-redshift Main-Sequence Galaxies
We present the first results of an ALMA survey of the lower fine structure
line of atomic carbon [C I](^3P_1\,-\,^{3}P_0) in far infrared-selected
galaxies on the main sequence at in the COSMOS field. We compare our
sample with a comprehensive compilation of data available in the literature for
local and high-redshift starbursting systems and quasars. We show that the [C
I]() luminosity correlates on global scales with the
infrared luminosity similarly to low- CO transitions. We report
a systematic variation of L'_{\rm [C\,I]^3P_1\,-\, ^3P_0}/ as a
function of the galaxy type, with the ratio being larger for main-sequence
galaxies than for starbursts and sub-millimeter galaxies at fixed .
The L'_{\rm [C\,I]^3P_1\,-\, ^3P_0}/ and / mass ratios are similar for main-sequence galaxies and for
local and high-redshift starbursts within a 0.2 dex intrinsic scatter,
suggesting that [C I] is a good tracer of molecular gas mass as CO and dust. We
derive a fraction of %
of the total carbon mass in the atomic neutral phase. Moreover, we estimate the
neutral atomic carbon abundance, the fundamental ingredient to calibrate [C I]
as a gas tracer, by comparing L'_{\rm [C\,I]^3P_1\,-\, ^3P_0} and available
gas masses from CO lines and dust emission. We find lower [C I] abundances in
main-sequence galaxies than in starbursting systems and sub-millimeter
galaxies, as a consequence of the canonical and gas-to-dust
conversion factors. This argues against the application to different galaxy
populations of a universal standard [C I] abundance derived from highly biased
samples.Comment: 14 pages + Appendix. Accepted for publication in ApJ. All the data
tables in Appendix will be also released in electronic forma
Testing Diagnostics of Nuclear Activity and Star Formation in Galaxies at z>1
We present some of the first science data with the new Keck/MOSFIRE
instrument to test the effectiveness of different AGN/SF diagnostics at z~1.5.
MOSFIRE spectra were obtained in three H-band multi-slit masks in the GOODS-S
field, resulting in two hour exposures of 36 emission-line galaxies. We compare
X-ray data with the traditional emission-line ratio diagnostics and the
alternative mass-excitation and color-excitation diagrams, combining new
MOSFIRE infrared data with previous HST/WFC3 infrared spectra (from the 3D-HST
survey) and multiwavelength photometry. We demonstrate that a high [OIII]/Hb
ratio is insufficient as an AGN indicator at z>1. For the four X-ray detected
galaxies, the classic diagnostics ([OIII]/Hb vs. [NII]/Ha and [SII]/Ha) remain
consistent with X-ray AGN/SF classification. The X-ray data also suggest that
"composite" galaxies (with intermediate AGN/SF classification) host bona-fide
AGNs. Nearly 2/3 of the z~1.5 emission-line galaxies have nuclear activity
detected by either X-rays or the classic diagnostics. Compared to the X-ray and
line ratio classifications, the mass-excitation method remains effective at
z>1, but we show that the color-excitation method requires a new calibration to
successfully identify AGNs at these redshifts.Comment: 7 pages, 4 figures. Accepted to ApJ Letter
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