908 research outputs found
Molecular line probes of activity in galaxies
The use of specific tracers of the dense molecular gas phase can help to
explore the feedback of activity on the interstellar medium (ISM) in galaxies.
This information is a key to any quantitative assessment of the efficiency of
the star formation process in galaxies. We present the results of a survey
devoted to probe the feedback of activity through the study of the excitation
and chemistry of the dense molecular gas in a sample of local universe
starbursts and active galactic nuclei (AGNs). Our sample includes also 17
luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs). From the
analysis of the LIRGs/ULIRGs subsample, published in Gracia-Carpio et al.(2007)
we find the first clear observational evidence that the star formation
efficiency of the dense gas, measured by the L_FIR/L_HCN ratio, is
significantly higher in LIRGs and ULIRGs than in normal galaxies. Mounting
evidence of overabundant HCN in active environments would even reinforce the
reported trend, pointing to a significant turn upward in the Kennicutt-Schmidt
law around L_FIR=10^11 L_sun. This result has major implications for the use of
HCN as a tracer of the dense gas in local and high-redshift luminous infrared
galaxies.Comment: 4 pages, 2 figures, contributed paper to Far-Infrared Workshop 07
(FIR 2007
Full two-photon downconversion of just a single photon
We demonstrate, both numerically and analytically, that it is possible to
generate two photons from one and only one photon. We characterize the output
two photon field and make our calculations close to reality by including
losses. Our proposal relies on real or artificial three-level atoms with a
cyclic transition strongly coupled to a one-dimensional waveguide. We show that
close to perfect downconversion with efficiency over 99% is reachable using
state-of-the-art Waveguide QED architectures such as photonic crystals or
superconducting circuits. In particular, we sketch an implementation in circuit
QED, where the three level atom is a transmon
Metric properties of Baumslag-Solitar groups
© 2015 World Scientific Publishing Company. We compute estimates for the word metric of Baumslag-Solitar groups in terms of the Britton's lemma normal form. As a corollary, we find lower bounds for the growth rate for the groups BS(p, q) with 1 < p ≤ q
Insights into the Carbon chemistry of Mon R2
Aiming to learn about the chemistry of the dense PDR around the ultracompact
(UC) HII region in Mon R2, we have observed a series of mm-wavelength
transitions of C3H2 and C2H. In addition, we have traced the distribution of
other molecules, such as H13CO+, SiO, HCO, and HC3N. These data, together with
the reactive ions recently detected, have been considered to determine the
physical conditions and to model the PDR chemistry. We then identified two kind
of molecules. The first group, formed by the reactive ions (CO+, HOC+) and
small hydrocarbons (C2H, C3H2), traces the surface layers of the PDR and is
presumably exposed to a high UV field (hence we called it as "high UV", or
HUV). HUV species is expected to dominate for visual absorptions 2 < Av < 5
mag. A second group (less exposed to the UV field, and hence called "low UV",
or LUV) includes HCO and SiO, and is mainly present at the edges of the PDR (Av
> 5 mag). While the abundances of the HUV molecules can be explained by gas
phase models, this is not the case for the studied LUV ones. Although some
efficient gas-phase reactions might be lacking, grain chemistry sounds like a
probable mechanism able to explain the observed enhancement of HCO and SiO.
Within this scenario, the interaction of UV photons with grains produces an
important effect on the molecular gas chemistry and constitutes the first
evidence of an ionization front created by the UC HII region carving its host
molecular cloud. The physical conditions and kinematics of the gas layer which
surrounds the UC HII region were derived from the HUV molecules. Molecular
hydrogen densities > 4 10^6 cm^(-3) are required to reproduce the observations.
Such high densities suggest that the HII region could be pressure-confined by
the surrounding high density molecular gas.Comment: 32 pages, 8 figures. Accepted by Astrophysical Journa
Widespread HCO emission in the M82's nuclear starburst
We present a high-resolution (~ 5'') image of the nucleus of M82 showing the
presence of widespread emission of the formyl radical (HCO). The HCO map, the
first obtained in an external galaxy, reveals the existence of a structured
disk of ~ 650 pc full diameter. The HCO distribution in the plane mimics the
ring morphology displayed by other molecular/ionized gas tracers in M82. More
precisely, rings traced by HCO, CO and HII regions are nested, with the HCO
ring lying in the outer edge of the molecular torus. Observations of HCO in
galactic clouds indicate that the abundance of HCO is strongly enhanced in the
interfaces between the ionized and molecular gas. The surprisingly high overall
abundance of HCO measured in M82 (X(HCO) ~ 4x10^{-10}) indicates that its
nuclear disk can be viewed as a giant Photon Dominated Region (PDR) of ~ 650 pc
size. The existence of various nested gas rings, with the highest HCO abundance
occurring at the outer ring (X(HCO) ~ 0.8x10^{-9}), suggests that PDR chemistry
is propagating in the disk. We discuss the inferred large abundances of HCO in
M82 in the context of a starburst evolutionary scenario, picturing the M82
nucleus as an evolved starburst.Comment: 13 pages, 3 figures, to appear in ApJ Letters; corrected list of
author
Jet-disturbed molecular gas near the Seyfert 2 nucleus in M51
Previous molecular gas observations at arcsecond-scale resolution of the
Seyfert 2 galaxy M51 suggest the presence of a dense circumnuclear rotating
disk, which may be the reservoir for fueling the active nucleus and obscures it
from direct view in the optical. However, our recent interferometric CO(3-2)
observations show a hint of a velocity gradient perpendicular to the rotating
disk, which suggests a more complex structure than previously thought. To image
the putative circumnuclear molecular gas disk at sub-arcsecond resolution to
better understand both the spatial distribution and kinematics of the molecular
gas. We carried out CO(2-1) and CO(1-0) line observations of the nuclear region
of M51 with the new A configuration of the IRAM Plateau de Bure Interferometer,
yielding a spatial resolution lower than 15 pc. The high resolution images show
no clear evidence of a disk, aligned nearly east-west and perpendicular to the
radio jet axis, as suggested by previous observations, but show two separate
features located on the eastern and western sides of the nucleus. The western
feature shows an elongated structure along the jet and a good velocity
correspondence with optical emission lines associated with the jet, suggesting
that this feature is a jet-entrained gas. The eastern feature is elongated
nearly east-west ending around the nucleus. A velocity gradient appears in the
same direction with increasingly blueshifted velocities near the nucleus. This
velocity gradient is in the opposite sense of that previously inferred for the
putative circumnuclear disk. Possible explanations for the observed molecular
gas distribution and kinematics are that a rotating gas disk disturbed by the
jet, gas streaming toward the nucleus, or a ring with another smaller counter-
or Keplarian-rotating gas disk inside.Comment: 5 pages, 4 figures, to appear in A&A Letters Special Issue for the
new extended configuration at the IRAM PdB
Molecular gas chemistry in AGN. II. High-resolution imaging of SiO emission in NGC1068: shocks or XDR?
This paper is part of a multi-species survey of line emission from the
molecular gas in the circum-nuclear disk (CND) of the Seyfert 2 galaxy NGC1068.
Single-dish observations have provided evidence that the abundance of silicon
monoxide(SiO) in the CND of NGC1068 is enhanced by 3-4 orders of magnitude with
respect to the values typically measured in quiescent molecular gas in the
Galaxy. We aim at unveiling the mechanism(s) underlying the SiO enhancement. We
have imaged with the IRAM Plateau de Bure interferometer the emission of the
SiO(2-1) and CN(2--1) lines in NGC1068 at 150pc and 60pc spatial resolution,
respectively. We have also obtained complementary IRAM 30m observations of HNCO
and methanol (CH3OH) lines. SiO is detected in a disk of 400pc size around the
AGN. SiO abundances in the CND of (1-5)xE-09 are about 1-2 orders of magnitude
above those measured in the starburst ring. The overall abundance of CN in the
CND is high: (0.2-1)xE-07. The abundances of SiO and CN are enhanced at the
extreme velocities of gas associated with non-circular motions close to the AGN
(r<70pc). Abundances measured for CN and SiO, and the correlation of CN/CO and
SiO/CO ratios with hard X-ray irradiation, suggest that the CND of NGC1068 has
become a giant X-ray dominated region (XDR). The extreme properties of
molecular gas in the circum-nuclear molecular disk of NGC1068 result from the
interplay between different processes directly linked to nuclear activity.
Whereas XDR chemistry offers a simple explanation for CN and SiO in NGC1068,
the relevance of shocks deserves further scrutiny. The inclusion of dust grain
chemistry would help solve the controversy regarding the abundances of other
molecular species, like HCN, which are under-predicted by XDR models.Comment: 18 pages, 13 figures, 2 tables; accepted for publication in A&
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