toward the quasar PKS 1830
211
N
and vibrationally excited C
H in IRC +10216
: Imaging the Dynamics of a Quasar Host Galaxy Through a Cosmic Lens
emission in a 
quasar host galaxy
for the AGILE GRB 080514B
and HCN absorption
CO 2-1 map of M51 with HERA: II. Total gas surface densities and gravitational stability
, Torsten Böker
, David S. Meier
and Daniela Calzetti
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany,
European Space Agency, Department RSSD, Keplerlaan 1, 2200 AG Noordwijk, Netherlands,
David S. Meier is a Jansky Fellow of the NRAO,
National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA,
Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 
pc. The
morphology of the tracers suggests that the molecular gas flow caused
by a large-scale stellar bar has been strongly affected by the
mechanical feedback from recent star formation activity within the
central 100 pc in the nucleus of the galaxy. Possibly, stellar winds
and/or supernova shocks originating in the nuclear star cluster have
compressed, and likely pushed outward, the infalling molecular gas,
thus significantly reducing the gas supply to the central
10 pc. Although our analysis currently lacks kinematic confirmation
due to the face-on orientation of IC 342, the described scenario is
supported by the generally observed repetitive nature of star
formation in the nuclear star clusters of late-type spiral galaxies.
Appeared in ApJ 684, L21
, T. Le Bertre, E. Gérard and J.M. Winters
LERMA, UMR 8112, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France,
GEPI, UMR 8111, Observatoire de Paris, 5 Place J. Janssen, 92195 Meudon Cedex, France,
IRAM, 300 rue de la Piscine, 38406 St. Martin d'Hères, France 
pc, possibly
more), and different complementary tracers are needed to describe
their global properties.
rotational line from RXLep. The line
profile is parabolic and implies an expansion velocity of 
kms
and a mass-loss rate
yr (
pc). The HI line at 21 cm
was detected with the Nançay Radiotelescope on the star
position and at several offset positions. The linear shell size
is relatively small, 
0.1 pc, but we detect a trail
extending southward to 0.5 pc. The line profiles are
approximately Gaussian with an FWHM 
km and
interpreted with a model developed for the detached shell around
the carbon-rich AGB star YCVn. Our HI spectra are
well-reproduced by assuming a constant outflow (
yr) of
years duration, which has been slowed down by the external medium.
The spatial offset of the HI source is consistent with
the northward direction of the proper motion measured by
Hipparcos, lending support to the presence of a trail resulting
from the motion of the source through the ISM, as already
suggested for Mira, RSCnc, and other sources detected in HI. The source was also observed in SiO (3 mm) and OH (18 cm),
but not detected.
Appeared in A&A 491, 789
, Schödel R., Baganoff F.K., Morris M., Bertram T., Dovciak M.,
Downes D., Duschl W.J.
, Karas V., König S., Krichbaum T.
, Krips M.
, Kunneriath D.,
Lu R.-S.
, Markoff S.
, Mauerhan J., Meyer L., Moultaka J.
, Muzic K., Najarro F.
,
Schuster K.F., Sjouwerman L.
, Straubmeier C., Thum C., Vogel S.
, Wiesemeyer H.
,
Witzel G., Zamaninasab M., Zensus A.
University of Cologne, Zülpicher Str. 77, D-50937 Cologne, Germany,
Instituto de Astrofísica de Andalucía, Camino Bajo de Huétor 50, 18008 Granada, Spain,
Center for Space Research, MIT, Cambridge, MA 02139-4307, USA,
Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1547, USA,
Astronomical Institute, Academy of Sciences, Bocdní II, CZ-14131 Prague, Czech Republic,
IRAM, Domaine Universitaire, 38406 St. Martin d'Hères, France,
Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15 24118 Kiel, Germany ,
Steward Observatory, The University of Arizona, 933 N. Cherry Ave. Tucson, AZ 85721, USA,
MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany,
Harvard-Smithsonian Center for Astrophysics, SMA project, 60 Garden Street, MS 78 Cambridge, MA 02138, USA,
Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098SJ Amsterdam, the Netherlands,
Observatoire Midi-Pyrénées, 14, Avenue Edouard Belin, 31400 Toulouse, France,
Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Cientificas, CSIC, Serrano 121, 28006 Madrid, Spain,
NRAO, PO Box 0, Socorro, NM 87801, USA,
Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA,
IRAM, Avenida Divina Pastora, 7, Núcleo Central, E-18012 Granada, Spain 
super-massive black hole (SMBH) at the Galactic
Center. The goal of these coordinated multi-wavelength observations is
to investigate the variable emission from Sgr A* in order to obtain a
better understanding of the underlying physical processes in the
accretion flow/outflow. The observations have been carried out using
the NACO adaptive optics (AO) instrument at the European Southern
Observatory's Very Large Telescope (July 2005, May 2007) and the
ACIS-I instrument aboard the Chandra X-ray Observatory (July 2005). We
report on a polarized NIR flare synchronous to a
erg/s X-ray
flare in July 2005, and a further flare in May 2007 that shows the
highest sub-flare to flare contrast observed until now. The
observations can be interpreted in the framework of a model involving
a temporary disk with a short jet. In the disk component flux density
variations can be explained due to hot spots on relativistic orbits
around the central SMBH. The variations of the sub-structures of the
May 2007 flare are interpreted as a variation of the hot spot
structure due to differential rotation within the disk.
Appeared in: J. of Physics: Conf. Series, V 131, Proc. of ``The Universe Under the Microscope - Astrophysics at High Angular Resolution'', p. 012002 (2008).
, N. Biver, E. Jehin, A.L. Cochran, H. Wiesemeyer,
J. Manfroid, D. Hutsemékers, C. Arpigny, J. Boissier, W. Cochran,
P. Colom, J. Crovisier, N. Milutinovic, R. Moreno, J.X. Prochaska,
I. Ramirez, R. Schulz, and J.-M. Zucconi
LESIA, Observatoire de Paris, 5 Place Jules Janssen, F-92190, Meudon, France,
Institut d'Astrophysique et de Géophysique, Sart-Tilman, B-4000, Liège, Belgium,
Department of Astronomy and McDonald Observatory, University of Texas at Austin, C-1400, Austin, USA,
IRAM, Avenida Divina Pastora, 7, Núcleo Central, E-18012 Granada, Spain,
IRAM, 300 rue de la Piscine, Domaine Universitaire, F-38406, Saint Martin d'Hères, France,
Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria BC V8P 5C2, Canada,
Department of Astronomy and Astrophysics, and UCO/Lick Observatory, University of California, 1156 High Street, Santa Cruz, CA 95064, USA,
ESA/RSSD, ESTEC, P.O. Box 299, NL-2200 AG Noordwijk, The Netherlands,
Observatoire de Besançon, F-25010 Besançon Cedex, France 
N/
N=139
26 in HCN, and
N/N=16540 in CN, establishing that HCN has the same
non-terrestrial isotopic composition as CN. The same conclusion is obtained
for the long-period comet C/1995 O1 (Hale-Bopp) after a reanalysis of
previously published measurements. These results are compatible with HCN
being the prime parent of CN in cometary atmospheres. The N excess
relative to the Earth atmospheric value indicates that N-bearing volatiles
in the solar nebula underwent important N isotopic fractionation at some
stage of Solar System formation. HCN molecules never isotopically
equilibrated with the main nitrogen reservoir in the solar nebula before
being incorporated in Oort-cloud and Kuiper-belt comets. The
C/
C ratios in HCN and CN are measured to be consistent with
the terrestrial value.
Appeared in ApJ 679, L49
, N. Biver, D. Bockelée-Morvan, and P. Colom
LESIA, Observatoire de Paris, 5 place Jules Janssen, F-92195 Meudon, France Comets are classified from their orbital characteristics into two separate classes: i) nearly-isotropic, mainly long-period comets and ii) ecliptic, short-period comets, the so-called Jupiter-family comets. These two classes apparently come from two different reservoirs, respectively the Oort cloud and the trans-Neptunian scattered disc. Due to their different history and -- possibly -- their different origin, they may have different chemical and physical properties that are worth being investigated.
The present article reviews the contribution of radio observations to our knowledge of the Jupiter-family comets (JFCs). The difficulty of such a study is the commonly low gas and dust productions of these comets. Long-period, nearly-isotropic comets from the Oort cloud are better known from Earth-based observations. On the other hand, Jupiter-family comets are more easily accessed by space missions. However, unique opportunities to observe Jupiter-family comets are offered when these objects come by chance close to the Earth (like 73P/Schwassmann-Wachmann 3 in 2006), or when they exhibit unexpected outbursts (as did 17P/Holmes in 2007).
About a dozen JFCs were successfully observed by radio techniques up to now.
Four to ten molecules were detected in five of them. No obvious evidence for
different properties between JFCs and other families of comets is found, as far
as radio observations are concerned.
Accepted for publication in Planetary & Space Science
, D. Bockelée-Morvan, N. Biver, J.
Crovisier, and H. Rickman
LESIA, Observatoire de Paris, 5 place Jules Janssen, F-92195 Meudon, France,
Astronomiska Observatoriet, Box 515, S-75120 Uppsala, Sweden 
=2-1) line in the comet with an
unprecedented sensitivity and spatial coverage, and a high spectral resolution
(20 kHz, i.e., 25 m s). A 36-point map, 60 by
, was obtained in
June 2003, and a 25-point map, 96 by
, in January 2004.
The CO emission line has a characteristic asymmetric profile. Our
analysis is based on a coma model, where the outgassing pattern is
derived from the shape of this line at the central position of the
map. When comparing to the observations, both maps show a line
intensity at offset positions which is 2-3 times stronger than the
model prediction. Different explanations to this are evaluated, and
it is found that for the global coma character, an extremely low gas
temperature in the inner coma reproduces the observed radial profile.
A cold inner coma depletes the population of the CO 
rotational
level in the region closest to the nucleus, making spectra observed at
offset positions relatively stronger. From the global appearance of
the maps, the coma was found to be largely axisymmetric, and the
presence of a strong extended source of CO, as indicated from earlier
observations using the SEST telescope, was not seen. When examining
the maps in more detail, a possible exception to this was seen in an
area
south of the comet, where an excess in emission is present
in both maps. Model fits to the spectra based on the cold inner coma
that we find, with an initial kinetic temperature 
= 4 K,
give a measure of 
, the CO production rate. was
found to be
mol s in June 2003,
and
mol s in January 2004. These
values are a factor 1.5 higher than that derived using only the
information available from non-mapped data, and this adjustment
applies also to previously published production rates.
Appeared in A&A 484, 537
|
toward the quasar PKS 1830211
- Guélin M. 
Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), P.O. Box 23-141, Taipei, 106, Taiwan,
Institut de Radio Astronomie Millimétrique (IRAM), 300 rue de la Piscine, F-38406 St Martin d'Hères, France,
Ecole Normale Supérieure/LERMA, 24 rue Lohmond, F-75005 Paris, France
spiral galaxy on the line of sight to the radio-loud gravitationally
lensed quasar PKS 1830211 reveals spectacular changes in the
HCO
and HCN line profiles. The depth of the absorption
toward the quasar NE image increased by a factor of 
in
1998-1999 and subsequently decreased by a factor 
between 2003
and 2006 (Fig 10). These changes were echoed by similar
variations in the absorption line wings toward the SW image. Most
likely, these variations result from a motion of the quasar images
with respect to the foreground galaxy, which could be due to a new
ejected source component: VLBA observations have shown that the
separation between the NE and SW images changed in 1997 by as much as
0.2 mas within a few months. Assuming that motions of similar
amplitude occurred in 1999 and 2003, we argue that the clouds
responsible for the NE absorption and the broad wings of the SW
absorption should be sparse and have characteristic sizes of 
pc.
Appeared in A&A 491, 739
![\includegraphics[angle=0,width=8.cm]{jan09-fig1.eps}](img133.gif) |
N and vibrationally excited CH in IRC +10216
, M. Guélin, M. Agúndez, M. C. McCarthy
and P. Thaddeus
DAMIR, Instituto de Estructura de la Materia, CSIC, Serrano 121, 28006 Madrid, Spain,
Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 St. Martin d'Hères, France,
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, U.S.A.,
School of Engineering and Applied Sciences, Harvard University, 29 Oxford Street, Cambridge, MA 02138, U.S.A. H and
CN (Fig. 12). Three of the series have half-integer rotational quantum
numbers; we assign them to the 
and 
vibronic
states of CH in its lowest (
) bending mode. The fourth
series, B1389, has integer J with no evidence of fine or hyperfine
structure; it has a rotational constant of 1388.860(2) MHz and a
centrifugal distortion constant of 33(1) Hz; it is almost certainly
CN.
N, which has not been observed so far in the
laboratory, is the 5th anion detected in interstellar space. Its
abundance is found to be fairly high relative to that of its neutral
counterpart (between 1/8 and 1/2.)
Appeared in ApJ 688, L83
|
: Imaging the Dynamics of a Quasar Host Galaxy Through a Cosmic Lens
, Fabian Walter, Brendon J. Brewer, Christopher L. Carilli,
Geraint F. Lewis, Frank Bertoldi, and Pierre Cox
MPIA, Königstuhl 17, Heidelberg, D-69117, Germany,
Astronomy Department, California Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125,
Hubble Fellow,
Institute of Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia,
NRAO, P.O. Box O, Socorro, NM 87801,
Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, Bonn, D-53121, Germany,
IRAM, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France 
) Very Large Array imaging of the
molecular gas in the host galaxy of the high-redshift quasar PSS
J2322+1944 (). These observations confirm that the molecular gas
(CO) in the host galaxy of this quasar is lensed into a full Einstein
ring and reveal the internal gas dynamics in this system. The ring has
a diameter of
and thus is sampled over 
resolution elements
by our observations. Through a model-based lens inversion, we recover
the velocity gradient of the molecular reservoir in the quasar host
galaxy of PSS J2322+1944. The Einstein ring lens configuration enables
us to zoom in on the emission and to resolve scales down to
kpc. From the model-reconstructed source, we find that the molecular
gas is distributed on a scale of 5 kpc and has a total mass of
. A basic estimate of the dynamical mass gives
, that is, only 
times the molecular gas
mass and 
times the black hole mass (assuming that the dynamical
structure is highly inclined). The lens configuration also allows us
to tie the optical emission to the molecular gas emission, which
suggests that the active galactic nucleus does reside within, but not
close to the center of, the molecular reservoir. Together with the (at
least partially) disturbed structure of the CO, this suggests that the
system is interacting. Such interaction, possibly caused by a major
``wet'' merger, may be responsible for both feeding the quasar and
fueling the massive starburst of
yr in this system, in
agreement with recently suggested scenarios of quasar activity and
galaxy assembly in the early universe.
Appeared in ApJ 686, 851
, Chris L. Carilli, Jeff Wagg, Frank Bertoldi, Fabian Walter, Karl M. Menten,
Alain Omont, Pierre Cox, Michael A. Strauss, Xiaohui Fan,
Linhua Jiang and Donald P. Schneider
Department of Astronomy, Peking University, Beijing 100871, China,
National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801,
Argelander-Institut für Astronomie, University of Bonn, Auf dem Hügel 71,53121 Bonn, Germany,
Max Planck Institute for Astronomy, Königsstuhl 17, 69117 Heidelberg,Germany,
MPIfR, Auf dem Hügel 71, 53121 Bonn,Germany,
Institut d'Astrophysique de Paris, CNRS, and Universite Pierre et MarieCurie, Paris, France,
IRAM, F-38406 St.Martin d'Hères, France,
Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544,
Steward Observatory, University of Arizona, Tucson, AZ 85721,
Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802. 
quasars at
250 GHz and 14 quasars at 1.4 GHz.We summarize all recent millimeter
and radio observations of the sample of the 33 quasars known with
and present a study of the rest-frame
far-infrared (FIR) properties of this sample. These quasars were
observed with the Max Planck Millimeter Bolometer Array (MAMBO) at
250 GHz with mJy sensitivity, and 30% of them were detected.We also
recover the average 250 GHz flux density of the MAMBO undetected
sources at 
by stacking the on-source measurements. The
derived mean radio-to-UV spectral energy distributions (SEDs) of the
full sample and the 250 GHz nondetections show no significant
differences from lower redshift optical quasars. Obvious FIR excesses
are seen in the individual SEDs of the strong 250 GHz detections, with
FIR-to-radio emission ratios consistent with those of typical
star-forming galaxies. Most 250 GHz- detected sources follow the
relationship derived from a sample of local
IR-luminous quasars (
), while the average
ratio of the nondetections is consistent with that
of the optically selected PG quasars. The MAMBO detections also tend
to have weaker Ly
emission than the nondetected sources.We
discuss possible FIR dust-heating sources and critically assess the
possibility of active star formation in the host galaxies of the
quasars. The average star formation rate of the MAMBO
nondetections is likely to be less than a few hundred
yr, but in the strong detections, the host galaxy star
formation is probably at a rate of
yr, which
dominates the FIR dust heating.
Appeared in ApJ 687, 848
, R. Neri, F. Bertoldi,, Ian Smail,,
T. R. Greve,, D. Trethewey,, A. W. Blain,, P. Cox,,
R. Genzel,, R. J. Ivison,
, A. Kovacs,, A. Omont, and A. M. Swinbank
Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK,
University of Victoria, Victoria, BC, V8W 3P6, Canada,
IRAM, St. Martin d'Hères, France,
MPIfR, Bonn, Germany,
Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK,
Astronomy Department, MPIA, Königsstuhl 17, D-69117 Heidelberg, Germany,
California Institute of Technology, Pasadena, CA 91125,
MPE, Garching, Germany,
UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK,
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK,
Institut d'Astrophysique de Paris, CNRS, Université de Paris, Paris, France 
m, appear to represent a
different population from the ultraluminous submillimeter-bright
population. They may be star-forming galaxies with hotter dust
temperatures, or they may have lower far-infrared luminosities and
larger contributions from obscured active galactic nuclei (AGNs). Here
we present observations of three examples of this
population, which we term ``submillimeter-faint radio galaxies''
(SFRGs; RG J163655, RG J131236, and RG J123711) in CO
using the
IRAM Plateau de Bure Interferometer to study their gas and dynamical
properties.We estimate the molecular gas mass in each of the three
SFRGs (
,
, and
, respectively) and, in the case of RG J163655, a dynamical
mass by measurement of the width of the CO line (
). While these gas masses are substantial, on
average they are 4 times lower than submillimeter-selected galaxies
(SMGs). Radio-inferred star formation rates
(
SFR
yr) suggest much
higher star formation efficiencies than are found forSMGs and shorter
gas depletion timescales (
Myr), much shorter than the time
required to form their current stellar masses (
Myr;
). By contrast, star formation rates (SFRs) may be
overestimated by factors of a few, bringing the efficiencies in line
with those typically measured for other ultraluminous star-forming
galaxies and suggesting that SFRGs are more like ultraviolet-selected
(UV-selected) star-forming galaxies with enhanced radio emission. A
tentative detection of RG J163655 at 
m suggests hotter dust
temperatures, and thus gas-to-dust mass fractions, similar to the
SMGs.
Appeared in ApJ 689, 889
emission in a quasar host galaxy
, Axel Weiss, Dominik A. Riechers
, Christopher L. Carilli,
Frank Bertoldi, Pierre Cox, and Karl M. Menten
MPIA, Königstuhl 17, Heidelberg, D-69117, Germany,
MPIfR, Auf dem Hügel 69, Bonn, D-53121, Germany,
Astronomy Department, California Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125, USA,
NRAO, P.O. Box O, Socorro, NM 87801, USA,
Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, Bonn, D-53121, Germany,
IRAM, 300 Rue de la Piscine, Domaine Universitaire, F-38406 Saint Martin d'Hères, France 
ground-state fine structure line at 
m of ionized nitrogen ([N
II]) in one of the highest-redshift quasars (J1148+5251
at 
) using the IRAM 30 m telescope. The line is not
detected at a (
) depth of 0.47 Jy km s, corresponding
to a [N II] luminosity limit of
![$L_{[N II]} < 4.0\times10^8
\mbox{L$_\odot$}$](img175.gif){kind=small}
and a
![$L_{[N ii]}/L_{FIR}$](img176.gif){kind=small}
ratio of
. In
parallel, we have observed the CO (
) line in J1148+5251,
which is detected at a flux level consistent with earlier
interferometric observations. Using our earlier measurements of the [C
II] 
m line strength, we derive an upper limit for the [N II]/[C II] line luminosity ratio of 
in
J1148+5251. Our upper limit for the [C II]/[N II] ratio is
similar to the value found for our Galaxy and M82 (the only
extragalactic system where the [N II] line has been detected
to date). Given the nondetection of the [N II] line we can
only speculate whether or not high-z detections are within reach of
currently operating observatories. However, [N II] and other
fine-structure lines will play a critical role in characterizing the
interstellarmedium at the highest redshifts (
) using the Atacama
Large Millimeter/submillimeter Array, for which the highly excited
rotational transitions of CO will be shifted outside the accessible
(sub-)millimeter bands.
Appeared in ApJ 691, L1
, A. Weiss, D. Downes, F. Walter, C. Henkel, and K. M. Menten
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China,
MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany,
IRAM, Domaine Universitaire, 38406 St-Martin-d'Hères, France,
MPIA, Königstuhl 17, 69117 Heidelberg, Germany 
) and the CO 
,
, 
, 
transitions as well as the dust continuum
at 3 and 1.2 mm towards the distant luminous infrared galaxy IRAS
F10214+4724 at 
. The C I(
) line is detected for
the first time towards this source and IRAS F10214+4724 now belongs to
a sample of only 3 extragalactic sources at any redshift where both of
the carbon fine structure lines have been detected. The source is
spatially resolved by our C I(
) observation and we detect
a velocity gradient along the east-west direction. The CI line ratio
allows us to derive a carbon excitation temperature of 
K.
The carbon excitation in conjunction with the CO ladder and
the dust continuum constrain the gas density to
cm
and the kinetic temperature to
K, similar
to the excitation conditions found in nearby starburst galaxies. The
rest-frame 
m dust continuum morphology is more compact than
the line emitting region, which supports previous findings that the
far infrared luminosity arises from regions closer to the active
galactic nucleus at the center of this system.
Appeared in A&A 491, 747
, and 92 international co-authors
Department of Astronomy and Astrophysics, 525 Davey Laboratory,
Pennsylvania State University, University Park, Pennsylvania 16802, USA 
ray bursts (GRBs) release copious amounts of
energy across the entire electromagnetic spectrum, and so provide a
window into the process of black hole formation from the collapse of
massive stars. Previous early optical observations of even the most
exceptional GRBs (990123 and 030329) lacked both the temporal
resolution to probe the optical flash in detail and the accuracy
needed to trace the transition from the prompt emission within the
outflow to external shocks caused by interaction with the progenitor
environment. Here we report observations of the extraordinarily bright
prompt optical and ray emission of GRB080319B that provide
diagnostics within seconds of its formation, followed by broadband
observations of the afterglow decay that continued for weeks. We show
that the prompt emission stems from a single physical region, implying
an extremely relativistic outflow that propagates within the narrow
inner core of a two-component jet.
Appeared in Nature 455, 183
and 41 international co-authors
Instituto de Astrofísica de Andalucía del Consejo
Superior de Investigaciones Científicas (IAA-CSIC),
PO Box 03004, E-18080 Granada, Spain 
G. They are detected in our Galaxy either as
soft 
-ray repeaters or anomalous X-ray pulsars. Soft -ray
repeaters are a rare type of -ray transient sources that are
occasionally detected as bursters in the high-energy sky. No optical
counterpart to the -ray flares or the quiescent source has yet
been identified. Here we report multi-wavelength observations of a
puzzling source, SWIFT J195509+261406. We detected more than 40
flaring episodes in the optical band over a time span of three days,
and a faint infrared flare 11 days later, after which the source
returned to quiescence. Our radio observations confirm a Galactic
nature and establish a lower distance limit of 
kpc. We suggest
that SWIFT J195509+261406 could be an isolated magnetar whose bursting
activity has been detected at optical wavelengths, and for which the
long-term X-ray emission is short-lived. In this case, a new
manifestation of magnetar activity has been recorded and we can
consider SWIFT J195509+261406 to be a link between the `persistent'
soft -ray repeaters/anomalous X-ray pulsars and dim isolated
neutron stars.
Appeared in Nature 455, 506
for the AGILE GRB 080514B
and 30 international co-authors
Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany , which is consistent with the reported pseudo-redshift
based on gamma-ray data. We find that the afterglow properties of GRB 080514B do
not differ from those exhibited by the global sample of
long bursts. Compared with the long burst sample, we conclude that
this burst was special because of its high-energy emission properties,
even though both its afterglow and host galaxy are not remarkable in
any way. Obviously, high-energy emission in the gamma-ray band does
not automatically correlate with the occurrence of special features in
the corresponding afterglow light.
Appeared in A&A 491, L29
, T. P. Krichbaum, A. Witzel,
A. Kraus, S. Britzen, S. Bernhart,
C. M. V. Impellizzeri, I. Agudo
, J. Klare,
B. W. Sohn
, E. Angelakis, U. Bach
,
K. É. Gabányi
, E. Körding,
A. Pagels, J. A. Zensus, S. J. Wagner,
L. Ostorero
, H. Ungerechts, M. Grewing,
M. Tornikoski, A. J. Apponi,
B. Vila-Vilaró, L. M. Ziurys, and
R. G. Strom
MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany,
Dipartimento di Fisica, Università di Perugia, via A. Pascoli, 06123 Perugia, Italy,
INAF - Osservatorio Astronomico di Torino, via Osservatorio 20, 10025 Pino Torinese (TO), Italy,
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain,
Korea Astronomy & Space Science Institute, 61-1 Hwaam-dong, 305-348 Daejeon, Korea,
Hungarian Academy of Sciences Research Group for Physical Geodesy and Geodynamics, Budapest, Hungary,
FÖMI Satellite Geodetic Observatory, Budapest, Hungary,
School of Physics & Astronomy, University of Southampton, Southampton, Hampshire SO17 1BJ, UK,
Landessternwarte Heidelberg-Königstuhl, Königstuhl, 69117 Heidelberg, Germany,
Dipartimento di Fisica Generale ``Amedeo Avogadro'', Università degli Studi di Torino, via P. Giuria 1, 10125 Torino, Italy,
Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino, via P. Giuria 1, 10125 Torino, Italy,
IRAM, Avenida Divina Pastora 7, Local 20, 18012 Granada, Spain,
IRAM, 300 rue de la Piscine, Domaine Universitaire de Grenoble, 38406 Saint-Martin d'Hères, France,
Metsähovi Radio Observatory, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland,
Arizona Radio Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA,
University of Arizona, Steward Observatory, 933 N. Cherry Ave., Tucson, AZ 85721, USA,
ASTRON, Postbus 2, 7990 AA Dwingeloo; and Astronomical Institute, University of Amsterdam, The Netherlands 
) comparing
the radio-bands with the hard X-ray emission, as seen by INTEGRAL at
3-200 keV.
day time scale amplitude increase of up to
%, systematically more pronounced towards shorter
wavelengths. The cross-correlation analysis reveals systematic
time-lags with the higher frequencies varying earlier, similar to
canonical variability on longer time-scales. The increase of the
variability amplitudes with frequency contradicts expectations from
standard interstellar scintillation (ISS) and suggests a
source-intrinsic origin for the observed inter-day variability. We
find an inverted synchrotron spectrum peaking near 90 GHz, with the
peak flux increasing during the first 4 days. The lower limits to TB
derived from the inter-day variations exceed the 1012 K IC-limit by up
to 3-4 orders of magnitude. Assuming relativistic boosting, our
different estimates of yield robust and self-consistent lower
limits of
- in good agreement with
obtained from VLBI studies and the IC-Doppler factors
obtained from the INTEGRAL data.
Appeared in A&A 490, 1019
, S. Guilloteau, V. Piétu, E. Chapillon, F.Gueth,
T. Henning, R. Launhardt, Y. Pavlyuchenkov,
K. Schreyer, and D. Semenov
LAB, UMR 5804, Observatoire de Bordeaux, 2 rue de l'Observatoire, 33270 Floirac, France,
IRAM, 300 rue de la Piscine, 38400 Saint Martin d'Hères, France,
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany,
Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, 07745 Jena, Germany ) observations with a high S/N per channel of the
CO 
and C
O and of the CO 
lines. A standard parametric disk model is used to fit the line data
in the Fourier-plane and to derive the CO disk properties. Our
measurement is based on a detailed analysis of the spectroscopic
profile from the CO disk rotating in Keplerian velocity. The
millimeter continuum, tracing the dust, is also analyzed.
AU at the
level. The hole manifests itself by a lack of emission
beyond the (projected) Keplerian speed at the inner radius. We also
constrain the temperature gradient in the disk.
AU). The frequent finding of inner
cavities suggests that either binarity is the most common scenario of
star formation in Taurus or that giant planet formation starts early.
Appeared in A&A 490, L15
, S. Guilloteau, D. Semenov, A. Bacmann, E. Chapillon, A. Dutrey,
F. Gueth, T. Henning, F. Hersant, R. Launhardt, J. Pety, and V. Piétu
Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, 07745 Jena, Germany,
Université Bordeaux 1, Laboratoire d'Astrophysique de Bordeaux (LAB), France,
CNRS/INSU - UMR 5804, BP 89, 33270 Floirac, France,
MPIA, Königstuhl 17, 69117 Heidelberg, Germany,
IRAM, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France 
H, CHOH, HCO, and CO isotopes. Using an iterative
minimization technique, observed columns densities and abundances are
derived. These values are further compared with results of an advanced
chemical model that is based on a steady-state flared disk structure
with a vertical temperature gradient, and gas-grain chemical network
with surface reactions.
in the 
transition,
tentatively detect HCN, and do not detect CS, CH, and
CHOH. The observed HCO and CO column densities as
well as the upper limits to the column densities of HCN, CS, CH,
and CHOH are in good agreement with modeling results and those
from previous studies.
Appeared in A&A 491, 821
, R. Schödel, M. García-Marín, G. Witzel, A. Weiss,
F. K. Baganoff, M. R. Morris, T. Bertram,
M. Dovciak
6, W. J. Duschl, V. Karas,
S. König, T. P. Krichbaum, M. Krips
, D. Kunneriath, R.-S. Lu
,
S. Markoff, J. Mauerhan, L.Meyer, J. Moultaka,
K.Muzic, F. Najarro, J.-U. Pott
, K. F. Schuster,
L. O. Sjouwerman, C. Straubmeier, C. Thum, S. N. Vogel,
H. Wiesemeyer, M. Zamaninasab, and J. A. Zensus
I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany,
MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany,
Instituto de Astrofísica de Andalucía, Camino Bajo de Huétor 50, 18008 Granada, Spain,
Center for Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA,
Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1547, USA,
Astronomical Institute, Academy of Sciences, Bocní II, 14131 Prague, Czech Republic,
Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15, 24118 Kiel, Germany,
Steward Observatory, The University of Arizona, 933 N. Cherry Ave. Tucson, AZ 85721, USA,
Harvard-Smithsonian Center for Astrophysics, SMA project, 60 Garden Street, MS 78 Cambridge, MA 02138, USA,
Astronomical Institute ``Anton Pannekoek'', University of Amsterdam, Kruislaan 403, 1098SJ Amsterdam, The Netherlands,
LATT, Université de Toulouse, CNRS, 14 avenue Édouard Belin, 31400 Toulouse, France,
DAMIR, Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Científicas, Serrano 121, 28006 Madrid, Spain,
W.M. Keck Observatory (WMKO), CARA, 65-1120 Mamalahoa Hwy., Kamuela, HI-96743, USA,
IRAM, Domaine Universitaire, 38406 Saint-Martin d'Hères, France,
National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA,
Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA,
IRAM, Avenida Divina Pastora, 7, Núcleo Central, 18012 Granada, Spain 
)
black hole at the Galactic center.
NIR. Inspection and modeling of the light curves show that
the sub-mm follows the NIR emission with a delay of 
h. We explain the flare emission delay by an adiabatic expansion of
the source components. The derived physical quantities that describe
the flare emission give a source component expansion speed of
c, source sizes around one Schwarzschild radius with flux
densities of a few Janskys, and spectral indices of 
to
1.8, corresponding to particle spectral indices 
to 4.6. At
the start of the flare the spectra of these components peak at
frequencies of a few THz.
or the expanding material contributes to a corona or disk,
confined to the immediate surroundings of Sgr A*.
Appeared in A&A 492, 337
, C. Codella, S. Viti, R. Neri and R. Cesaroni
Universitat de Barcelona, Departament d'Astronomia i Meteorologia, Unitat Associada a CSIC, Martí
i Franquès 1, 08028 Barcelona, Catalunya, Spain,
INAF, Istituto di Radioastronomia, Sezione di Firenze, Largo E. Fermi 5, I-50125 Firenze, Italy,
Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK,
IRAM, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France,
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy OHCHO) toward the hot molecular core G31.41+0.31
through IRAM PdBI observations at 1.4, 2.1, and 2.9 mm. The
CHOHCHO emission comes from the hottest (
K) and densest
(
cm) region closest (
AU) to
the (proto)stars. The comparison of data with gas-grain chemical
models of hot cores suggests for G31.41+0.31 an age of a few 
yr. We also show that only small amounts of CO need to be processed on
grains in order for existing hot core gas-grain chemical models to
reproduce the observed column densities of glycolaldehyde, making
surface reactions the most feasible route to its formation.
Appeared in ApJ 690, L93
and HCN absorption
, J. Pety, and R. Lucas
NRAO, 520 Edgemont Road, Charlottesville, VA, 22903-2475, USA.
IRAM, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France,
Obs. de Paris, 61 Av. de l'Observatoire, 75014 Paris, France H, CH, HCO,
and NH, which have relative abundances that are strikingly similar to
those inferred toward the dark cloud TMC-1.
rotational
transitions of A- and E- CHOH near 96.740 GHz and used the VLA to
search for the 
transition of HCN at 21.3 GHz.
OH nor HCN were detected at column
densities well below those of all polyatomics known in diffuse clouds
and somewhat below the levels expected from comparison with TMC-1. The
HCN/HCN ratio is at least 3 - 10 times higher in diffuse gas than
toward TMC-1.
Appeared in A&A 486, 493
, R. Lucas, and H. S. Liszt
IRAM, 300 Rue de la Piscine, 38406 Saint Martin d'Hères, France
Obs. de Paris, 61 Av. de l'Observatoire, 75014 Paris, France,
NRAO, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA 
resolution single-dish maps of 
CO and 
emission
over a
by
field; ii) a hybrid (interferometer+ single dish)
aperture synthesis mosaic of CO emission at 
resolution over a
-diameter region.
resolution, the CO emission toward
NRAO150 is 30 - 100% brighter at some velocities than seen
previously with 
resolution, and there are some modest systematic
velocity gradients over the
field. Of the five CO components seen
in the absorption spectra, the weakest ones are absent in emission
toward NRAO150 but appear more strongly at the edges of the region
mapped in emission. The overall spatial variations in the strongly
emitting gas have Poisson statistics with rms fluctuations about equal
to the mean emission level in the line wings and much of the line
cores. The
line ratios calculated
pixel-by-pixel cluster around 0.7. At
resolution, disparity between
the absorption and emission profiles of the stronger components has
been largely ameliorated. The CO emission exhibits i)
remarkably bright peaks,
K, even as
from NRAO150;
ii) smaller relative levels of spatial fluctuation in the line cores,
but a very broad range of possible intensities at every velocity; and
iii) striking kinematics whereby the monotonic velocity shifts and
supersonically broadened lines in spectra are decomposed into
much stronger velocity gradients and abrupt velocity reversals of
intense but narrow, probably subsonic, line cores.
resolution toward NRAO 150 remain undetected at
resolution. This
implies that they are not a previously-hidden large-scale molecular
component revealed in absorption, but they do highlight the robustness
of the chemistry into regions where the density and column density are
too low to produce much rotational excitation, even in CO. Bright CO
lines around NRAO150 most probably reflect the variation of a chemical
process, i.e. the C
CO conversion. However, the ultimate cause of the
variations of this chemical process in such a limited field of view
remains uncertain.
Appeared in A&A 489, 217
, S. Guilloteau, A. Dutrey, and V. Piétu
Université Bordeaux 1, Laboratoire d'Astrophysique de Bordeaux (LAB),
UMR 5804, 2 rue de l'Observatoire, BP 89, 33270 Floirac, France,
CNRS/INSU - UMR 5804, BP 89, 33270 Floirac, France,
IRAM, 300 rue de la Piscine, 38400 Saint Martin d'Hères, France transition. The disk properties are derived using
a standard disk model. We use the Meudon PDR code to study the
chemistry.
, challenges previous interpretations given for UX
Ori - like luminosity variations of this star.
Appeared in A&A 488, 565
and F. Combes
IRAM, Domaine Universitaire,
300 rue de la piscine, 38400 St Martin d'Hères, France,
LERMA, Observatoire de Paris, 61 av. de l'Observatoire, 75014 Paris, France 
for each pointing in
MS0735.6+7421, and a few
in M87. This non detection means
that either the cooling is strongly reduced by the AGN feedback or
that the gas is cooling in very localized places like thin filaments,
possibly diluted in the large beam for MS0735.6+7421. For M87, the
AGN heating appears to have stopped the cooling completely.
Appeared in A&A 489, 101
, H. Wiesemeyer, C. Thum, A. Belloche, and K. M. Menten
MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany,
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 72, Cambridge, MA 02138, USA,
IRAM, Avenida Divina Pastora 7, Local 20, 18012 Granada, Spain,
IRAM, Rue de la Piscine, 38406 Saint Martin d'Hères, France O, G34.3+0.2, and UYSO 1 dense molecular
cloud cores in transitions of rare CO isotopologues and CS. The
feasibility of such observations had to be established by studying the
influence of polarized sidelobes, e.g., in the presence of extended
emission in the surroundings of compact sources.
% was found in the CS line toward G34.3+0.2.
Appeared in A&A 492, 757
, Villata M., Larionov V.M., Gurwell M.A., Chen W.P., Kurtanidze O.M.,
Aller M.F., Böttcher M., Calcidese P., Hroch F., Lähteenmäki A., Lee C.-U.,
Nilsson K., Ohlert J., Papadakis I.E.
, Agudo I., Aller H.D., Angelakis E.
,
Arkharov A.A., Bach U., Bachev R.
Berdyugin A., Buemi C.S.
, Carosati D.
,
Charlot P.
, Chatzopoulos E., Forné E.
, Frasca A., Fuhrmann L., Gómez J.L.,
Gupta A.C.
; Hagen-Thorn V.A., Hsiao W.-S., Jordan B.
, Jorstad S.G.
, Konstantinova T.S.,
Kopatskaya E.N., Krichbaum T.P., Lanteri L., Larionova L.V., Latev G.
, Le Campion J.-F.,
Leto P.
, Lin H.-C., Marchili N., Marilli E., Marscher A.P., McBreen B.
, Mihov B.
,
Nesci R.
, Nicastro F.
, Nikolashvili M.G.
, Novak R.
, Ovcharov E., Pian E.
,
Principe D., Pursimo T.
, Ragozzine B., Ros J.A., Sadun A.C.
, Sagar R., Semkov E.,
Smart R.L., Smith N.
, Strigachev A., Takalo L.O., Tavani M.
, Tornikoski M., Trigilio C.,
Uckert K., Umana G., Valcheva A., Vercellone S.
, Volvach A.
and Wiesemeyer H.
INAF - Osservatorio Astronomico di Torino, Italy,
Astron. Inst., St.-Petersburg State Univ., Russia,
Pulkovo Observatory, St. Petersburg, Russia,
Harvard-Smithsonian Center for Astroph., Cambridge, MA, USA,
Institute of Astronomy, National Central University, Taiwan,
Abastumani Astrophysical Observatory, Georgia,
Department of Astronomy, University of Michigan, MI, USA,
Department of Physics and Astronomy, Ohio Univ., OH, USA,
Osservatorio Astronomico della Regione Autonoma Valle d'Aosta, Italy,
Inst. of Theor. Phys. and Astroph., Masaryk Univ., Czech Republic,
Metsähovi Radio Obs., Helsinki Univ. of Technology, Finland,
Korea Astronomy and Space Science Institute, South Korea,
Tuorla Observatory, Univ. of Turku, Piikkiö, Finland,
Michael Adrian Observatory, Trebur, Germany,
IESL, FORTH, Heraklion, Crete, Greece,
Physics Department, University of Crete, Greece,
Instituto de Astrofíisica de Andalucía (CSIC), Granada, Spain,
MPIfR, Bonn, Germany,
Inst. of Astronomy, Bulgarian Academy of Sciences, Sofia, Bulgaria,
INAF - Osservatorio Astrofisico di Catania, Italy,
Armenzano Astronomical Observatory, Italy,
Université de Bordeaux, Observatoire Aquitain des Sciences de l'Univers, Floirac, France,
CNRS, Laboratoire d'Astrophysique de Bordeaux, UMR 5804, Floirac, France,
Agrupació Astronòmica de Sabadell, Spain,
ARIES, Manora Peak, Nainital, India,
School of Cosmic Physics, Dublin Institute For Advanced Studies, Ireland,
Institute for Astrophysical Research, Boston University, MA, USA,
Sofia University, Bulgaria,
INAF - Istituto di Radioastronomia, Sezione di Noto, Italy,
School of Physics, University College Dublin, Ireland,
Dept. of Phys. ``La Sapienza'' Univ, Roma, Italy,
INAF - Osservatorio Astronomico di Roma, Italy,
Abastumani Astrophysical Observatory, Georgia,
N. Copernicus Observatory and Planetarium in Brno, Czech Republic,
INAF - Osservatorio Astronomico di Trieste, Italy,
Nordic Optical Telescope, Santa Cruz de La Palma, Spain,
Dept. of Phys., Univ. of Colorado Denver, Denver, CO USA,
Cork Institute of Technology, Cork, Ireland,
INAF, IASF-Roma, Italy,
INAF, IASF-Milano, Italy,
Radio Astronomy Lab. of Crimean Astrophysical Observatory, Ukraine,
IRAM Granada, Spain 
and possibly turns into a bluer-when-brighter trend in bright
states. This behaviour is due to the interplay of different emission
components, the synchrotron one possibly being characterised by an
intrinsically variable spectrum. All the near-IR spectra show a
prominent H emission line (
Å), whose flux
appears nearly constant, indicating that the broad line region is not
affected by the jet emission. We show the broad-band SEDs
corresponding to the epochs of the XMM-Newton pointings and compare
them to those obtained at other epochs, when the source was in
different brightness states. A double power-law fit to the EPIC
spectra including extra absorption suggests that the soft-X-ray
spectrum is concave, and that the curvature becomes more pronounced as
the flux decreases. This connects fairly well with the UV excess,
which becomes more prominent with decreasing flux. The most obvious
interpretation implies that, as the beamed synchrotron radiation from
the jet dims, we can see both the head and the tail of the big blue
bump. The X-ray flux correlates with the optical flux, suggesting that
in the inverse-Compton process either the seed photons are synchrotron
photons at IR-optical frequencies or the relativistic electrons are
those that produce the optical synchrotron emission. The X-ray
radiation would thus be produced in the jet region from where the
IR-optical emission comes.
Appeared in A&A 491, 755
, Troland T.H., Crutcher R.M., Paubert G.
LERMA/LRA, CNRS UMR 8112, École Normale Supérieure and Observatoire de Paris, 24 rue Lhomond, 75231 Paris Cedex 05, France,
University of Kentucky, Department of Physics and Astronomy, Lexington, KY 40506, USA,
University of Illinois, Department of Astronomy, Urbana, IL 61801, USA,
IRAM, 7 avenida Divina Pastora, Granada, Spain 
lines in the direction of 14 regions of star
formation.
mG while the average density of the medium sampled is
cm. We show that the CN line probably samples
regions similar to those traced by CS and that the magnetic field
observed mostly pervades the dense cores. The dense cores are found to
be critical to slightly supercritical with a mean mass-to-flux ratio
to 4 with respect to critical. Their turbulent and
magnetic energies are in approximate equipartition.
Appeared in A&A 487, 247
, Paubert G., Moreno R., Moullet A.
LESIA, Observatoire de Paris, 92195 Meudon Cedex, France,
IRAM, Granada, Spain 
km), performed in support of Venus Express, and based on CO
millimeter observations. Most observations, sampling the CO and
CO
lines, were acquired with the IRAM 30-m telescope, over four
distinct periods: (i) Summer 2006; (ii) May June 2007, in association
with the coordinated ground-based campaign; (iii) August 2007 inferior
conjunction and (iv) September 2007. In the latter period, additional
measurements (CO) were obtained with the APEX 12-m
telescope. Overall, the measurements indicate a large body of temporal
variability of the Venus mesospheric field, but general features
emerge: (i) winds strongly increase with altitude within the
mesosphere, by a factor of 
over a decade in pressure; (ii) many,
but not all, of our observations can be viewed as the superposition of
zonal retrograde and subsolar-to-antisolar (SSAS) flows of comparable
speeds, typically 
m/s near 0.1 mbar (
km) and 
m/s near 0.01 mbar (
km) (iii) the wind field was very stable
over three consecutive observing days in May June 2007, but much more
variable on a similar time base in August 2007 (iv) at a 
km resolution, the nightside wind field appears very complex,
with evidence that the SSAS flow does not reach high latitudes, and
possible evidence for additional meridional winds. Our Summer 2006
observations, which sample Venus' dayside, seem to suggest that a
prograde zonal flow is superimposed to the SSAS circulation for this
period. This surprising result, which implies a pre-midnight
convergence of the wind field, requires confirmation, and fruitful
comparisons may be obtained from the analysis of motions in the O
emission images, as observed by Venus Express.
Appeared in: Planetary and Space Science 56, 1355
, S.G. Jorstad
,
A.P. Marscher, C.M. Raiteri, M. Villata,
I. Agudo, M.F. Aller, A.A. Arkharov,
I. M. Asfandiyarov, U. Bach, R. Bachev,
A. Berdyugin, M. Böttcher, C. S. Buemi,
P. Calcidese, D. Carosati, P. Charlot,
W.-P. Chen, A. Di Paola, M. Dolci,
S. Dogru, V. T. Doroshenko
,
Yu. S. Efimov, A. Erdem, A. Frasca,
L. Fuhrmann, P. Giommi, L. Glowienka,
A. C. Gupta
, M. A. Gurwell,
V. A. Hagen-Thorn, W.-S.Hsiao,
M. A. Ibrahimov, B. Jordan, M. Kamada,
T. S. Konstantinova, E. N. Kopatskaya,
Y. Y. Kovalev
, Y. A. Kovalev,
O. M. Kurtanidze, A. Lähteenmäki, L. Lanteri,
L. V. Larionova, P. Leto, P. Le Campion,
C.-U. Lee, E. Lindfors, E. Marilli,
I. McHardy, M. G. Mingaliev, S. V. Nazarov,
E. Nieppola, K. Nilsson, J. Ohlert,
M. Pasanen, D. Porter, T. Pursimo,
J. A. Ros, K. Sadakane, A. C. Sadun,
S. G. Sergeev
, N. Smith, A. Strigachev,
N. Sumitomo, L. O. Takalo, K. Tanaka,
C. Trigilio, G. Umana, H. Ungerechts
,
A. Volvach, and W. Yuan
Astron. Inst., St.-Petersburg State Univ., Russia,
Pulkovo Observatory, St.-Petersburg, Russia,
INAF, Osservatorio Astronomico di Torino, Italy,
Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain,
Department of Astronomy, University of Michigan, MI, USA,
MPIfR, Bonn, Germany,
Inst. of Astron., Bulgarian Acad. of Sciences, Sofia, Bulgaria,
Department of Physics and Astronomy, Ohio Univ., OH, USA,
Oss. Astronomico della Regione Autonoma Valle d'Aosta, Italy,
Armenzano Astronomical Observatory, Italy,
Lab. d'Astrophys., Univ. Bordeaux 1, CNRS, Floirac, France,
Institute of Astronomy, National Central University, Taiwan,
INAF, Osservatorio Astronomico di Roma, Italy,
INAF, Osservatorio Astronomico di Collurania Teramo, Italy,
COMU Observatory, Turkey,
INAF, Osservatorio Astrofisico di Catania, Italy,
Department of Phys. and Astron. Univ. of Aarhus, Denmark,
YNAO, Chinese Academy of Sciences, Kunming, PR China,
Harvard-Smithsonian Center for Astroph., Cambridge, MA, USA,
Ulugh Beg Astron. Inst., Tashkent, Uzbekistan,
Inst. for Astrophys. Research, Boston Univ., MA, USA,
Astronomical Institute, Osaka Kyoiku University, Japan,
Astro Space Centre of Lebedev Physical Inst., Moscow, Russia,
Abastumani Astrophysical Observatory, Georgia,
Metsähovi Radio Obs., Helsinki Univ. of Technology, Finland,
Korea Astronomy and Space Science Institute, South Korea,
University of Southampton, UK,
Tuorla Observatory, Univ. of Turku, Piikkiö, Finland,
Michael Adrian Observatory, Trebur, Germany,
Cardiff University, Wales, UK,
Nordic Optical Telescope, Santa Cruz de La Palma, Spain,
Agrupació Astronòmica de Sabadell, Spain,
Dept. of Phys., Univ. of Colorado, Denver, USA,
Crimean Astrophysical Observatory, Ukraine,
Radio Astron. Lab. of Crimean Astroph. Observatory, Ukraine,
ASI Science Data Centre, Frascati, Italy,
INAF, Istituto di Radioastronomia, Sezione di Noto, Italy,
School of Cosmic Physics, Dublin Inst. for Adv. Studies, Ireland,
Cork Institute of Technology, Cork, Ireland,
Moscow Univ., Crimean Lab. of Sternberg Astron. Inst., Ukraine,
Isaac Newton Institute of Chile, Crimean Branch, Ukraine,
Special Astrophysical Observatory, N. Arkhyz, Russia,
IRAM Granada, Spain,
ARIES, Manora Peak, Nainital, India 
, while in the 
keV X-ray band it varies
in slope from 
to . The steepest X-ray spectrum
occurs at a flux minimum. During a decline in flux from maximum in
late 2006, the optical and 43 GHz core polarization vectors rotate by
.
that is steepened to 
at high energies by
radiative losses. The X-ray emission at flux minimum comes most likely
from a new component that starts in an upstream section of the jet
where inverse Compton scattering of seed photons from outside the jet
is important. The rotation of the polarization vector implies that the
jet contains a helical magnetic field that extends pc past
the 43 GHz core.
Appeared in A&A 492, 389
, Benford Dominic J., Allen Christine A., Maher Stephen F.,
Sharp Elmer H., Ames Troy J., Arendt Richard G., Chuss David T.,
Dwek Eli, Fixsen Dale J., Miller Tim M.
, Moseley S. Harvey,
Navarro Santiago, Sievers Albrecht and Wollack Edward J.
NASA Goddard Space Flight Ctr., USA,
Univ. of Maryland, College Park, USA,
Science Systems & Applications, USA,
Global Science & Technology, USA,
Univ. of Maryland Baltimore County, USA,
MEI Technologies, USA,
IRAM Granada, Spain 
BUG bolometer array with 2 mm-pitch detectors for astronomical
observations using our 2 mm wavelength camera GISMO (the Goddard IRAM
Superconducting 2 Millimeter Observer) at the IRAM 30m telescope in
Spain. The 2 mm spectral range provides a unique terrestrial window
enabling ground-based observations of the earliest active dusty
galaxies in the universe and thereby allowing a better constraint on
the star formation rate in these objects. We present preliminary
results from our observing run with the first fielded BUG bolometer
array and discuss the performance of the instrument.
Appeared in: Mm and Sub-mm Detectors and Instrumentation for Astronomy IV. Eds Duncan, Holland, Withington, Jonas, Proc. of the SPIE Vol. 7020, 702004
, B. Ocaña, V. P. Kozhevnikov, D. Charbonneau, F. T. O'Donovan, and L. R. Doyle
Instituto de Astrofísica de Canarias, C. Via Lactea S/N, 38205 La Laguna, Tenerife, Spain,
IRAM, Av. Divina Pastora 7, Núcleo Central, 18012 Granada, Spain,
Astronomical Observatory, Ural State University, Lenin ave. 51, Ekaterinburg, 620083, Russia,
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA,
California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA,
SETI Institute, 515 N. Whisman Road, Mountain View, CA 94043, USA 
years or an object in the mass
range of 
to
with periods of hundreds to
thousands of years is the most likely origin of the observed minimum
timing behavior.
Appeared in A&A 480, 563
, C. Thum, R. Moreno and N. Yan
IRAM, 300 rue de la Piscine, 38406 St. Martin d`Hères, France,
LESIA (LAM -bat. 18), 5 Place Jules Janssen, 92195 Meudon Cedex, France,
Service d'Aeronomie CNRS/IPSL, 91371 Verrieres-le-Buisson, France 
Andrew allow
a separation of the data into 40
wide longitude intervals and by this
an investigation of the disk-averaged brightness temperature with Mercury's
longitude. From the new mm-wavelength data, and data taken from the literature,
we derive the disk-averaged brightness temperature as a function of wavelength.
On Mercury's night side a significant decrease in brightness temperature
occurs towards shorter wavelengths.
A&A, in print
, M. Bremer, G. Butin, M. Carter,
A. Greve, J.W. Lamb, B. Lazareff, J. Lopez-Perez,
F. Mattiocco, J. Peñalver and C. Thum
IRAM, St Martin d'Hères, France,
Raman Research Institute, Bangalore, India,
California Institute of Technology, OVRO, Big Pine, USA,
OAN, Centro Astronomico de Yebes, Guadalajara, Spain 
m
are described. This involved both phase retrieval and phase coherent
holography using a variety of radiation sources at several
frequencies. A finite-element model was utilised in improving the
temperature control system for the telescope structure. The factors
influencing the ultimate surface accuracy are discussed.
Appeared in: IET Microwaves, Antennas & Propagation, Feb. 2009, Vol.3, Issue 1, 99
, D.Riechers, P.Cox, R.Neri, C.Carilli,
F.Bertoldi, A.Weiss and R.Maiolino
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany,
IRAM, 300 rue de la Piscine, F-38406 St-Martin-d'Hères, France,
NRAO, PO Box O, Socorro, New Mexico 87801, USA,
Argelander Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany,
MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany,
L'Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Roma, I-00040 Monte Porzio Catone, Roma, Italy , when the Universe was less than a billion years old) has
an infrared luminosity of
times that of the Sun,
presumably significantly powered by a massive burst of star
formation. In local examples of extremely luminous galaxies, such as
Arp 220, the burst of star formation is concentrated in a relatively
small central region of 
pc radius. It is not known on which
scales stars are forming in active galaxies in the early Universe, at
a time when they are probably undergoing their initial burst of star
formation. We do know that at some early time, structures comparable
to the spheroidal bulge of the Milky Way must have formed. Here we
report a spatially resolved image of [CII] emission of the host galaxy
of J114816.64+525150.3 that demonstrates that its star-forming gas is
distributed over a radius of about 750 pc around the centre. The
surface density of the star formation rate averaged over this region
is 
yearkpc
. This surface density is
comparable to the peak in Arp 220, although about two orders of
magnitude larger in area. This vigorous star-forming event is likely
to give rise to a massive spheroidal component in this system.
Appeared in: Nature 457, 699
CO 2-1 map of M51 with HERA: II. Total gas surface densities and gravitational stability
, C. Kramer, K.F. Schuster, S. Garcia-Burillo, J. Stutzki
KOSMA, I. Physikalisches Institut, Universität zu Köln, Germany,
IRAM Granada, Spain,
IRAM Grenoble, France,
Observatorio de Madrid, Spain /HI
transition, the gas-to-dust ratios, and the stability of the disk
against gravitational collapse.
We combine maps of the molecular gas using CO 2-1 map
HERA/IRAM-30m data and HI VLA data to study the total gas surface
density and the phase transition of atomic to molecular gas. The total
gas surface density is compared to the dust surface density from
m SCUBA data. Taking into account the velocity dispersions
of the molecular and atomic gas, and the stellar surface densities
derived from the 2MASS K-band survey, we derive the total Toomre Q
parameter of the disk.
The gas surface density in the spiral arms is 
higher
compared to that of the interarm regions. The ratio of molecular to
atomic surface density shows a nearly power-law dependence on the
hydrostatic pressure 
. The gas surface density distribution
in M51 shows an underlying exponential distribution with a scale
length of 
kpc representing 55% of the total gas mass,
comparable to the properties of the exponential dust disk. In contrast
to the velocity widths observed in HI, the CO velocity dispersion
shows enhanced line widths in the spiral arms compared to the interarm
regions. The contribution of the stellar component in the Toomre
Q-parameter analysis is significant and lowers the combined
Q-parameter Q
by up to 70% towards the threshold for
gravitational instability. The value of Q varies from 
in
radial averages. A map of Q shows values around 1 on the
spiral arms indicating self-regulation at play.
Accepted for publication in A&A
H, C