466 research outputs found
86 GHz SiO maser survey of late-type stars in the Inner Galaxy. IV. SiO emission and infrared data for sources in the Scutum and Sagittarius-Carina arms, 20 deg < l < 50 deg
We present an 86 GHz SiO (v = 1, J = 2 ---> 1) maser search toward late-type
stars located within |b|<0.5 deg and 20 deg < l < 50 deg. This search is an
extension at longer longitudes of a previously published work. We selected 135
stars from the MSX catalog using color and flux criteria and detected 92 (86
new detections). The detection rate is 68%, the same as in our previous study.
The last few decades have seen the publication of several catalogs of point
sources detected in infrared surveys (MSX, 2MASS, DENIS, ISOGAL, WISE, GLIMPSE,
AKARI, and MIPSGAL). We searched each catalog for data on the 444 targets of
our earlier survey and for the 135 in the survey reported here. We confirm
that, as anticipated, most of our targets have colors typical of oxygen-rich
asymptotic giant branch (AGB) stars. Only one target star may have already left
the AGB. Ten stars have colors typical of carbon-rich stars, meaning a
contamination of our sample with carbon stars <=1.7%.Comment: 13 pages, 6 Figures, A&A accepte
The sub-millimeter properties of broad absorption line quasars
We have carried out the first systematic survey of the sub-millimeter
properties of broad absorption line (BAL) quasars. 30 BAL quasars drawn from a
homogeneously selected sample from the Sloan Digital Sky Survey at redshifts
2<z<2.6 were observed with the SCUBA array at the JCMT to a typical rms
sensitivity of 2.5 mJy. Eight quasars were detected at > 2 sigma significance,
four of which are at > 3 sigma significance. The far-infrared luminosities of
these quasars are > 10^{13} L_solar. There is no correlation of sub-millimeter
flux with either the strength of the broad absorption feature or with absolute
magnitude in our sample. We compare the sub-millimeter flux distribution of the
BAL quasar sample with that of a sample of quasars which do not show BAL
features in their optical spectra and find that the two are indistinguishable.
BAL quasars do not have higher sub-millimeter luminosities than non-BAL
quasars. These findings are consistent with the hypothesis that all quasars
would contain a BAL if viewed along a certain line-of-sight. The data are
inconsistent with a model in which the BAL phenomenon indicates a special
evolutionary stage which co-incides with a large dust mass in the host galaxy
and a high sub-millimeter luminosity. Our work provides constraints on
alternative evolutionary explanations of BAL quasars.Comment: 8 pages, 2 figures, ApJ, in pres
On the nature of infrared-faint radio sources in the SXDF and VLA-VVDS fields
Infrared-Faint Radio Sources (IFRSs) are an unusual class of objects that are
relatively bright at radio wavelengths but have faint or undetected infrared
counterparts even in deep surveys. We identify and investigate the nature of
IFRSs using deep radio (S 100 Jy beam at
5), optical (m 26 - 27.7 at 5), and near-IR
(S 1.3 - 2.0 Jy beam at 5) data
available in two deep fields namely the Subaru X-ray Deep Field (SXDF) and the
Very Large Array - VIMOS VLT Deep Survey (VLA-VVDS) field. In 1.8 deg of
the two fields we identify a total of nine confirmed and ten candidate IFRSs.
We find that our IFRSs are high-redshift radio-loud AGN, with 12/19 sources
having redshift estimates in the range of 1.7 - 4.3, while a limit
of 2.0 is placed for the remaining seven sources. Notably, our study
finds, for the first time, IFRSs with measured redshift 3.0, and also, the
redshift estimates for IFRSs in the faintest 3.6 m flux regime i.e.,
S 1.3 Jy. Radio observations show that our IFRSs
exhibit both compact unresolved as well as extended double-lobe morphologies,
and have predominantly steep radio spectra between 1.4 GHz and 325 MHz. The
non-detection of all but one IFRSs in the X-ray band and the optical-to-MIR
colour (m - m) suggest that a significant fraction
of IFRSs are likely to be hosted in dusty obscured galaxies.Comment: 20 pages, 8 figures, 4 tables, accepted for publication in MNRA
Experimental verification of minima in excited long-range Rydberg states of Rb_2
Recent theoretical studies with alkali atoms A excited to high
Rydberg states predicted the existence of ultra long-range molecular bound
states. Such excited dimers have large electric dipole moments which, in
combination with their long radiative lifetimes, make them excellent candidates
for manipulation in applications. This letter reports on experimental
investigations of the self-broadening of Rb principal series lines, which
revealed multiple satellites in the line wings. The positions of the satellites
agree quantitatively with theoretically-predicted minima in the excited
long-range Rydberg states of Rb.Comment: 3 figures, 5 pages in two-column forma
Interstellar extinction towards the inner Galactic Bulge
DENIS observations in the J (1.2 micron) and K_S (2.15 micron) bands together
with isochrones calculated for the RGB and AGB phase are used to draw an
extinction map of the inner Galactic Bulge. The uncertainty in this method is
mainly limited by the optical depth of the Bulge itself. A comparison with
fields of known extinction shows a very good agreement. We present an
extinction map for the inner Galactic Bulge (approx. 20 sq. deg.)Comment: 4 pages, 4 figures, accepted for publication in A&A as a letter, see
also http://www-denis.iap.fr/articles/extinction
Generalized Pseudopotentials for Higher Partial Wave Scattering
We derive a generalized zero-range pseudopotential applicable to all partial
wave solutions to the Schroedinger equation based on a delta-shell potential in
the limit that the shell radius approaches zero. This properly models all
higher order multipole moments not accounted for with a monopolar delta
function at the origin, as used in the familiar Fermi pseudopotential for
s-wave scattering. By making the strength of the potential energy dependent, we
derive self-consistent solutions for the entire energy spectrum of the
realistic potential. We apply this to study two particles in an isotropic
harmonic trap, interacting through a central potential, and derive analytic
expressions for the energy eigenstates and eigenvalues.Comment: RevTeX 4 pages, 1 figure, final published versio
86 GHz SiO masers in Galactic Centre OH/IR stars
We present results on a search for 86.243 GHz SiO (J = 2 -- 1, v = 1) maser
emission toward 67 OH/IR stars located near the Galactic Centre. We detected 32
spectral peaks, of which 28 correspond to SiO maser lines arising from the
envelopes of these OH/IR stars. In OH/IR stars, we obtained an SiO maser
detection rate of about 40%. We serendipitously detected two other lines from
OH/IR stars at 86.18 GHz, which could be due to a CCS-molecule transition at
86.181 GHz or probably to an highly excited OH molecular transition at 86.178
GHz. The detection rate of 86 GHz maser emission is found to be about 60% for
sources with The Midcourse Space Experiment (MSX) A - E < 2.5 mag; but it drops
to 25% for the reddest OH/IR stars with MSX A - E > 2.5 mag. This supports the
hypothesis by Messineo et al. (2002) that the SiO masers are primarily found in
relatively thinner circumstellar material.Comment: 4 figures, 14 page
Deep Galaxy survey at 6.75 micron with the ISO satellite
Deep 6.75um mid-IR ISOCAM observations were obtained of the Canada-France
Redshift Survey (CFRS) 1415+52 field with the Infrared Space Observatory. The
identification of the sources with optical counterparts is described in detail,
and a classification scheme is devised which depends on the S/N of the
detection and the inverse probability of chance coincidence. 83% of the 54
ISOCAM sources are identified with Iab<23.5 counterparts. The (I-K)ab colors,
radio properties, spectrophotometric properties and frequency of nuclear
activity of these counterparts differ on average from those of typical CFRS
galaxies. CFRS spectra are available for 21 of the sources which have Iab <=
22.5 (including 7 stars). Most of the strongest sources are stars or AGN. Among
the non--stellar counterparts with spectra, 40% are AGNs, and 53% are galaxies
that display star formation activity and/or significant contributions of A
stars. The ISOCAM sources also display an IR excess, even when compared with
heavily-reddened local starburst galaxies. An upper limit of 30% of
extragalactic ISO sources could be at z>1 of the 44 S6.75um > 150uJy sources
which are non-stellar (7 "spectroscopic" and 3 "photometric" stars excluded)Comment: 13 pages, 12 figures. Accepted for publication in A
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