3 research outputs found
Radio Recombination Lines at Decametre Wavelengths: Prospects for the Future
This paper considers the suitability of a number of emerging and future
instruments for the study of radio recombination lines (RRLs) at frequencies
below 200 MHz. These lines arise only in low-density regions of the ionized
interstellar medium, and they may represent a frequency-dependent foreground
for next-generation experiments trying to detect H I signals from the Epoch of
Reionization and Dark Ages ("21-cm cosmology"). We summarize existing
decametre-wavelength observations of RRLs, which have detected only carbon
RRLs. We then show that, for an interferometric array, the primary instrumental
factor limiting detection and study of the RRLs is the areal filling factor of
the array. We consider the Long Wavelength Array (LWA-1), the LOw Frequency
ARray (LOFAR), the low-frequency component of the Square Kilometre Array
(SKA-lo), and a future Lunar Radio Array (LRA), all of which will operate at
decametre wavelengths. These arrays offer digital signal processing, which
should produce more stable and better defined spectral bandpasses; larger
frequency tuning ranges; and better angular resolution than that of the
previous generation of instruments that have been used in the past for RRL
observations. Detecting Galactic carbon RRLs, with optical depths at the level
of 10^-3, appears feasible for all of these arrays, with integration times of
no more than 100 hr. The SKA-lo and LRA, and the LWA-1 and LOFAR at the lowest
frequencies, should have a high enough filling factor to detect lines with much
lower optical depths, of order 10^-4 in a few hundred hours. The amount of
RRL-hosting gas present in the Galaxy at the high Galactic latitudes likely to
be targeted in 21-cm cosmology studies is currently unknown. If present,
however, the spectral fluctuations from RRLs could be comparable to or exceed
the anticipated H I signals.Comment: 9 pages; Astron. & Astrophys., in pres
Carbon Recombination Lines from the Galactic Plane at 34.5 & 328 MHz
We present results of a search for carbon recombination lines in the Galaxy
at 34.5 MHz (C) made using the dipole array at Gauribidanur near
Bangalore. Observations made towards 32 directions, led to detections of lines
in absorption at nine positions. Followup observations at 328 MHz
(C) using the Ooty Radio Telescope detected these lines in emission.
A VLA D-array observation of one of the positions at 330 MHz yielded no
detection implying a lower limit of 10' for the angular size of the line
forming region.
The longitude-velocity distribution of the observed carbon lines indicate
that the line forming region are located mainly between 4 kpc and 7 kpc from
the Galactic centre. Combining our results with published carbon recombination
line data near 76 MHz (\nocite{erickson:95} Erickson \et 1995) we obtain
constraints on the physical parameters of the line forming regions. We find
that if the angular size of the line forming regions is , then
the range of parameters that fit the data are: \Te K, \ne \cm3 and pathlengths pc which may correspond to thin
photo-dissociated regions around molecular clouds. On the other hand, if the
line forming regions are in extent, then warmer gas (\Te K) with lower electron densities (\ne \cm3) extending
over several tens of parsecs along the line of sight and possibly associated
with atomic \HI gas can fit the data. Based on the range of derived parameters,
we suggest that the carbon line regions are most likely associated with
photo-dissociation regions.Comment: To appear in Journal of Astrophysics & Astronomy, March 200
Carbon and hydrogen radio recombination lines from the cold clouds towards Cassiopeia A
We use the Low Frequency Array to perform a systematic high spectral
resolution investigation of the low-frequency 33-78 MHz spectrum along the line
of sight to Cassiopeia A. We complement this with a 304-386 MHz Westerbork
Synthesis Radio telescope observation. In this first paper we focus on the
carbon radio recombination lines.
We detect Cn lines at -47 and -38 km s in absorption for
quantum numbers n=438-584 and in emission for n=257-278 with high signal to
noise. These lines are associated with cold clouds in the Perseus spiral arm
component. Hn lines are detected in emission for n=257-278. In
addition, we also detect Cn lines at 0 km s associated with the
Orion arm.
We analyze the optical depth of these transitions and their line width. Our
models show that the carbon line components in the Perseus arm are best fit
with an electron temperature 85 K and an electron density 0.04 cm and
can be constrained to within 15\%. The electron pressure is constrained to
within 20\%. We argue that much of these carbon radio recombination lines arise
in the CO-dark surface layers of molecular clouds where most of the carbon is
ionized but hydrogen has made the transition from atomic to molecular. The
hydrogen lines are clearly associated with the carbon line emitting clouds, but
the low-frequency upperlimits indicate that they likely do not trace the same
gas. Combining the hydrogen and carbon results we arrive at a firm lower limit
to the cosmic ray ionization rate of 2.510 s, but the
actual value is likely much larger.Comment: Accepted for publication in MNRAS, 29 pages, 15 figures and 7 table