Millimétrique Institut de Radioastronomie IRAM IRAM Annual Report 2010
30-meter diameter telescope, Pico Veleta
6 x 15-meter interferometer, Plateau de Bure
The Institut de Radioastronomie Millimétrique (IRAM) is a multi-national scientific institute covering all aspects of radio astronomy at millimeter wavelengths: the operation of two high-altitude observatories – a 30-meter diameter telescope on Pico Veleta in the Sierra Nevada (southern Spain), and an interferometer of six 15 meter diameter telescopes on the Plateau de Bure in the French Alps – the development of telescopes and instrumentation, radio astronomical observations and their interpretation.
IRAM was founded in 1979 by two national research organizations: the CNRS and the Max-Planck-Gesellschaft – the Spanish Instituto Geográfico IRAM Addresses: Nacional, initially an associate member, became a full member in 1990.
Institut de Radioastronomie The technical and scientific staff of IRAM develops instrumentation and Millimétrique 300 rue de la piscine, software for the specific needs of millimeter radioastronomy and for the Saint-Martin d’Hères benefit of the astronomical community. IRAM’s laboratories also supply F-38406 France Tel: +33 [0]4 76 82 49 00 devices to several European partners, including for the ALMA project. Fax: +33 [0]4 76 51 59 38 [email protected] www.iram.fr Front Cover IRAM’s scientists conduct forefront research in several domains of astrophysics, from nearby star-forming regions to objects at cosmological View of the Orion nebula, the closest Observatoire du Plateau de Bure distances. region of massive star forming Saint-Etienne-en-Dévoluy region, in the 12CO(2-1) emission, F-05250 France Tel: +33 [0]4 92 52 53 60 IRAM Partner Organizations: that traces the distribution of the
Fax: +33 [0]4 92 52 53 61 Centre National de la Recherche Scientifique (CNRS) – Paris, France 2010 Annual Report cold (10-100 K) molecular gas. The Max-Planck-Gesellschaft (MPG) – München, Deutschland map was obtained using HERA at the Instituto de Radioastronomía Instituto Geografico Nacional (IGN) – Madrid, España 30-meter telescope and has spatial Milimétrica resolution of 12” (or 0.025 pc). The Avenida Divina Pastora 7, Local 20, E-18012 Granada, España dynamics of the molecular gas are Tel: +34 958 80 54 54 shown in blue (for the emission with Fax: +34 958 22 23 63 [email protected] velocities between –5 and 8 km/s) and in red (for velocities between Observatorio 12 and 25 km/s). The map in green Radioastronómico shows the emission from warm de Pico Veleta Sierra Nevada, (100 to 1000 K) dust and gas at the Granada, España surface of the clouds, traced at 8 Tel: +34 958 48 20 02 Fax: +34 958 48 11 49 microns by the Midcourse Space Experiment satellite.
Designed and produced by rebusparis.com Printed in France (O. Berné et al. 2010) Annual report 2010 1
IRAM Annual Report 2010
Edited by Pierre Cox and Karin Zacher
With contributions from Michael Bremer, Frédéric Gueth, Bastien Lefranc, Roberto Neri, Laurent Palaric, Alain Perrigouard, Jérôme Pety, Karl-Friedrich Schuster, Marc Torres
Pico Veleta texts by Carsten Kramer with contributions from Walter Brunswig, Dave John, Javier Lobato, Santiago Navarro, Gabriel Paubert, Juan Peñalver, Salvador Sánchez, Clemens Thum, Hans Ungerechts, Helmut Wiesemeyer 2 Institut de Radioastronomie Milimétrique Annual report 2010 3
Contents
Introduction 5 Highlights of research with the IRAM telescopes in 2010 7
The Observatories 16 The 30-meter telescope 16 Plateau de Bure Interferometer 21
Grenoble Headquarters 27 SIS group 27 Frontend group 28 Backend group 32 Mechanical group 33 IRAM ARC node 34 Computer group 35 Science software activities 36 Public relations 37
Personnel and Finances 38 Income and expenditure 2010 – 2010 39
Annexes 40 Annex I - Telescope schedules 40 Annex II – Publications in 2010 48 Annex III – IRAM executive council and committee members 62 4 Institut de Radioastronomie Milimétrique Annual report 2010 5
Introduction
In the year 2010, both IRAM facilities underwent A major, high-risk action was undertaken in major enhancements. At the Plateau de Bure September 2010 at the 30-meter telescope with interferometer, the refurbishment of all antennas the installation of two new gearboxes (Azimuth with new precision-machined aluminum panels and Elevation) to replace the old ones that showed was successfully completed. Today the array is excessive vibrations and clear signs of ageing. After composed of six antennas with excellent surface careful inspection, it was decided to replace the accuracies of order 40 microns that enable obser four remaining gearboxes as well. This action will vation with maximum efficiency at the highest guarantee that the 30-meter telescope will continue available frequencies. This refurbishment is also to operate in an optimum way and remain the key in preparing the interferometer for the NOEMA best possible single-dish telescope for millimeter project (the greater stability of the aluminum panels observations. diminishing the maintenance time). With their continuous support for this refurbishment, the IRAM Continuing the trends seen in recent years, the Partners have allowed to maintain the observatory number of proposals that are submitted continues at a word-leading level and ensure the long-term to increase both at the 30-meter telescope and future of the interferometer. Another important the Plateau de Bure interferometer. The number of change that occurred in 2010 was the upgrade of proposals originating from countries outside of the the LO reference system from DRO to YIG-based IRAM Partner’s countries remains at a level of about oscillators, which has significantly improved the 30% of the observing time. This continuous increase phase noise. Finally, all the antennas were equipped in proposals is translated in the large number of with 345 GHz receivers that include electronically papers that are published based on or using IRAM tunable 1st Local Oscillators and modified versions data, that amount in 2010 to about 150 in total. It of the 2SB mixers developed for the ALMA Band 7, should be noted that the total number of papers providing excellent noise performance and a that includes IRAM personnel is exceptionally high 4 GHz IF bandwidth for each polarization. First in 2010 as a large number of papers are based on results obtained using these new receivers have data obtained with the Herschel satellite, a project demonstrated the potential of the Plateau de Bure in which IRAM has been involved at various levels. interferometer at high frequencies, yielding cutting- As in previous years, the topics cover the entire field edge scientific results, including the highest angular of modern astronomy, spanning the range from solar resolution observation (0.2”) yet achieved at Bure. system studies to observations of the first objects Some of these results are described in this report. that were formed in the universe, from the search of new complex or rare molecules to understanding At the 30-meter telescope, new Fourier Transform the processes of star formation, from constraining spectrometers were installed at the end of 2010 and the properties of the gas and dust in proto-planetary upgrades are planned for a 32 GHz instantaneous disks to detailed studies of the molecular gas in bandwidth. In the laboratory further progress has nearby galaxies. The availability of new instruments, been achieved in broadband receiver technology the increase in the characteristics of the back-ends with a recent spectacular development of a and the front-ends and the refurbishments at both sideband-separating mixer for the EMIR Band 3 that facilities each time have opened up new possibilities will extend the frequency range (200-280 GHz) and to study sources that are fainter, probe more double the continuum sensitivity. This will lead the efficiently than before the chemical complexity of way to increased sensitivities, observing speed and celestial objects or increase the speed by which flexibility, and consolidate the leading role of the studies can be done therefore enabling large scale 30-meter telescope for wideband spectral millimeter and more ambitious programs to be conducted. surveys and studies. During the summer of 2010, a prototype HEMT receiver operating at 3 mm Examples of scientific highlights are described in this was successfully tested at the 30-meter telescope, annual report, and include, for instance, the highest showing very good performance in both noise angular resolution map yet obtained at the Plateau and stability, and this receiver will serve as a test de Bure interferometer of a nearby proto-planetary platform for ongoing HEMT amplifier developments. disk, the detection of an emission line of water vapor 6 Institut de Radioastronomie Milimétrique
in a high-redshift, strongly lensed source that was so encouraging and stable that it could be made uncovered in the H-ATLAS deep survey of Herschel. available to the community for general use. These Another outstanding example is the detection of successful observing tests provide a useful basis for a new type of instability in the interstellar medium the building of a new generation large field of view that is the result of the interaction of massive stars bolometer camera for the 30-meter telescope. with the surrounding molecular gas. Concerning the ALMA Band 7 production, its pace Further enhancements are planned at both is fully sustained. A milestone was reached at the IRAM telescopes and all the technical groups end of 2010 when half of the 65 (and 8 spares) have continued their active work to increase the receivers, with state-of-the-art performances, were performances of the facilities and develop new delivered to and accepted by the ALMA project. instruments. In particular, the developments for a The production during the year 2010 amounted future heterodyne array receiver for the 30-meter to nineteen receivers. The project should normally telescope are actively pursued and the design of come to completion at the end of 2012. a 5x5 multibeam receiver for the 3 mm band is in good progress. The backend group is studying a new Planning the future of IRAM, the activity around generation (the 5th) correlator, including pioneering the NOEMA project gained further momentum work on multi-bit 8 GHz samplers that will eventually during 2010. In July 2010, an international Visiting lead to a flexible correlator as foreseen for NOEMA. Committee, chaired by Robert Wilson (Center for In view of replacing the MAMBO bolometer camera Astrophysics), reviewed the activities of IRAM and at the 30-meter telescope, further successful gave strong support for the NOEMA project. The observing tests were done with two bolometer report of the Visiting Committee provided the Three members of the IRAM Visiting Committee cameras. One, NIKA, is based on Kinetic Inductance basis for detailed discussions at the Partners’ level shown at their visit to the Plateau de Bure Detectors (KID) and build by a consortium of to explore how to best implement and build the interferometer in July 2009. institutes led by the Institut Néel (Grenoble) with a NOEMA project in a timely fashion. The Partners Standing in front of the recently installed WideX strong implication of IRAM. The recent observing agreed to make the necessary resources available correlator are, from left to right: Ewine F. van Dishoeck tests provided further very encouraging results in to start the project in a Phase 1 that will include the (Leiden Observatory, NL), Robert W. Wilson (CfA, both of the 2 and 1 mm windows. Further improve construction of a set of 4 antennas with receivers Cambridge, USA – Chair of ments will be made and new observations are and a new correlator. the Visiting Committee) and Catherine Cesarky (CEA, planned in the course of 2011. Another bolometer France). The other members of the Visiting Committee camera, GISMO, based on TES technology and The year 2010 was again a remarkable year with were: Christopher McKee build by the Goddard group at NASA, operates in many major achievements at both IRAM facilities: (University of Berkeley, USA) and Robert C. Kennicutt, Jr the 2mm window. This camera was recently tested projects were successfully completed, while others (Oxford University, UK). again at the 30-meter telescope with results that are were started or are under development; many out standing scientific results that are based on IRAM data have been published, including large and ambitious observing programs that have a high impact and visibility; the ongoing improvements that occur at all levels to keep the instrumentation up to date and plan for the future, gradually trans form the IRAM observatories into more efficient, versatile and outstanding facilities; last but not least, the positive decisions which were made by the IRAM Partners to expand the Plateau de Bure interferometer and transform it, in the next coming years, into the Northern Extended Millimeter Array, will have a profound and positive impact on the future of IRAM and its role in the ALMA era. Annual report 2010 7
Highlights of research with the IRAM telescopes in 2010
Herschel Gravitational characterize the nature of these high-z sources as lenses: IRAM follow-up well as the properties of the lensing galaxies. studies Prominent amongst these observations are those Gravitational lensed sources have played an done at sub/millimetre wavelengths. The strength important role in infrared and sub-millimetre studies of the sources detected by Herschel together with of high-redshift galaxies and active galactic nuclei recent technological developments at the sub- (AGN) since the discovery of FSC10214+4724 by the millimetre facilities has opened a new area. In IRAS satellite (Rowan-Robinson et al. 1991). Similar particular, the redshift of these sources, which are sources (including the Cloverleaf) triggered the sub- enshrouded in dust, can now directly be determined millimetre studies of galaxies in the early universe from the measurement of a series of CO lines. To date and allowed pioneering detections of the properties the distances to more than 10 sources uncovered in of these systems through observations of the the Herschel deep-field surveys have been measured emission of the dust continuum and the molecular using this technique, at the CSO and now APEX lines. In this new field, the IRAM facilities played a (with ZSpec), the GBT (with Zspectrometer), CARMA key role from the early 1990’s onward. The results and the Plateau de Bure interferometer (with the demonstrated the usefulness of strong gravitational newly installed correlator, WideX). As an example, magnification in the investigation of the detailed the redshift of the most prominent, highest redshift properties of distant galaxies. source found so far (ID.141) was ‘blindly’ determined at the Plateau de Bure interferometer, yielding a This observational field has recently received a new redshift z=4.24 (Cox et al. 2011). The detection of boost from the results released from the wide-field CO lines using the Plateau de Bure interferometer surveys done with the Herschel Space Observatory enabled robust redshift determination of five other – in particular, the H-ATLAS and HerMES projects that Herschel lensed sources in the redshift range 2 magnifications; double object lensing by the same deflector; radio-loud sources; or high-z masers. MM18423+5938: an Extremely Bright Galaxy in the Early Universe In the course of a program designed to search for debris left by the formation of planets around nearby stars, Lestrade and collaborators serendipitously discovered an extremely bright source, using MAMBO at the 30-meter telescope. Subsequent Spectrum of the water a maximum separation of 9”, revealing the internal follow-up spectroscopic observations showed emission in the Herschel source H-ATLAS ID.17b at gas dynamics in this system. that the source MM18423+5938 was a galaxy at z=2.3. The line corresponds to the para H₂O 2₀₂ -1₁₁ emission a redshift of z=3.93 undergoing vigorous, dust- line redshifted at 299 GHz. It Another example is the detection of water in the enshrouded star formation activity. Bright, star- was obtained at the Plateau de Bure interferometer using 202−111 transition of para-H₂O in the source H-ATLAS forming submillimeter galaxies (SMGs) trace the the newly installed band 4 receiver. ID.17b (z=2.3052), using the band 4 receiver at the most massive galaxies assembled during an active From Omont et al. 2011. A&A, Plateau de Bure interferometer (Omont et al. 2011) phase of galaxy formation, which peaked at a 530, L3 - confirming a previous, tentative detection done at redshift around ~2.5. Their star formation rate can the CSO (Lupu et al. 2011). The intrinsic water line be prodigious (up to 1000 M per year) and the luminosity in ID.17b is comparable to that of the underlying starburst activity is believed to result local ultra-luminous starburst galaxy Mrk231 and from major merger events. the excitation of the H₂O levels are probably similar in both objects. This detection shows that some of The apparent infrared luminosity of MM18423+5938 the Herschel lenses can harbour a rich chemistry that is estimated to be 4.8 1014 L and the inferred remains to be studied in the future with ALMA and apparent star formation rate is 8.3 104 M per year, NOEMA. about 50 times higher than for the most prolific star- forming galaxies known. The molecular hydrogen The examples of these recent studies provide us with gas (H2) fueling star formation was estimated to be a first glimpse of what can be expected in the future between 2.1011 and 11.1011 M, which is at least from this unique sample of hundreds of Herschel as large as in the most massive galaxies known but high-z lensed galaxies: today with Plateau de Bure, which are older and have had more time to build soon in the frame of the ALMA Early Science, and up their masses. All these values clearly point to later with the fully operational ALMA and NOEMA. gravitational amplification. The enhanced capabilities of the latter facilities will allow countless extensions for each of the topics To measure the redshift of MM18423+5938, Lestrade mentioned above, including: blind CO redshift et al. used EMIR, the multi-band heterodyne receiver determination and search for objects at the highest installed in 2010 at the 30-meter telescope. Its redshifts; high-resolution imaging and dynamics 7.4 GHz wide, dual linear polarization bandwidth of strongly lensed galaxies; comprehensive studies was used to search for emission lines of carbon of dark matter in high-z deflectors; high sensitivity monoxide. Several lines were detected which molecular (and atomic) spectroscopy; molecular enabled a robust determination of the redshift of gas in high-z Active Galactic Nuclei; search and this source. The 12CO line excitation was found to be study of exceptional, high-z lensed systems: highest moderate, suggesting that there is no strong heating Map of the molecular gas in the 5-4 transition of by a central AGN and that the starburst activity must CO (shown as contours) and the dust emission at be moderate. 890 microns (color image) towards the lensed galaxy HLSW-01 at z=2.95. The The galaxy MM18423+5938 must be amplified by a line data were obtained using the Plateau de Bure intervening massive and closely aligned foreground interferometer and the dust continuum was measured galaxy. High angular resolution observations using with the SubMillimeter interferometers at millimeter and radio wavelengths, Array (SMA) in Hawaii. The four spots of the lensed which should reveal the multiple mirror images image are clearly seen with a maximum separation of of MM18423+5938, are currently underway. These ~9”, revealing the internal observations will help to constrain the lensing and gas dynamics in this system. to study at high resolution the morphology and From Riechers et al. 2011, ApJ, 733, L12 Annual report 2010 9 the properties of the molecular gas where the star formation activity takes place. These data will also be useful to further understand how galaxies built up their masses and assembled their stellar populations early in cosmic time. Quasar Feedback Disclosed by Giant Molecular Outflows In the standard scenario for galaxy evolution, young star-forming galaxies transform into red bulge- dominated spheroids, where star formation has been quenched. To explain this transformation, a strong negative feedback generated by accretion onto a central super-massive black hole is often invoked. The depletion of gas resulting from quasar-driven outflows should eventually stop star-formation across the host galaxy and lead the black hole to “suicide” by starvation. Direct observational evidence for a major quasar feedback onto the host galaxy is still missing, because outflows previously observed in quasars are generally associated with the ionized component of the gas, which only accounts for a minor fraction of the total gas content, and typically feedback to highly supersonic shocks generated by EMIR spectra of the (4-3), occurs in the central, compact regions (on ~pc radiatively accelerated nuclear winds. In contrast, (6-5), and (7-6) transitions of ¹²CO and of the two CI scales). the contribution by supernovae associated with the lines revealing the presence starburst fall short by several orders of magnitude of a large gas reservoir at To investigate whether the fast outflows observed to account for the kinetic energy observed in the a redshift of 3.9296. The vertical scale is the main in the nearby active galactic nucleus (AGN) Mrk231 outflow. The direct observational evidence for quasar beam temperature (K). in the atomic gas phase are also affecting the feedback provides solid support to the scenarios molecular gas phase, Feruglio and collaborators ascribing the observed properties of local massive From Lestrade et al. 2010, A7A used the Plateau de Bure interferometer to perform galaxies to quasar-induced large-scale winds. 522, L4 a deep integration in the ¹²CO(1-0) emission line. Thanks to the correlator WideX, they succeeded in detecting the low surface-brightness wings of the line, with velocities of up to 750 km/s that are spatially resolved on a 1kpc scale. Despite several Left: HST/WFPC2 image previous observations of CO in Mrk231, these wings of Mrk231. Right: The broad line emission profile were never detected before, on one hand because detected in 12CO(1-0) of insufficient frequency band coverage, on the with the Plateau de Bure other because of the intrinsic low surface brightness Interferometer from the inner 1kpc. of the wings (the flux of the broad component is ~1/5 flux of the narrow core). Feruglio et al. suggest From Feruglio et al. 2010, A7A, 518, L155 that the broad wings trace a giant molecular outflow of about 700 M /yr, about 3-4 times larger than the ongoing star-formation rate observed in the host galaxy. The authors expect that the wind will expel the cold gas reservoir in about 10⁷ yr and halt the star-formation activity on the same timescale. The inferred kinetic energy in the molecular outflow is ~10⁴⁴ erg/s, corresponding to a few percent of the AGN bolometric luminosity, which is very close to the fraction expected by models ascribing quasar 10 Institut de Radioastronomie Milimétrique Cold Molecular Gas in the additional CO clumps showing non-circular motions Inner Two Kiloparsecs of are detected: one associated with the southern NGC 4151 feature and the other lying at about 600pc north of the nucleus. Finally, and very surprisingly, no cold NGC4151 is one the best studied nearby active molecular gas is detected in the central 300pc, galaxies and is sometimes referred to as the proto- where abundant near-infrared H₂ line emission typical Seyfert 1. Although it has been extensively is present. This suggests that either the H₂ line observed at all wavelengths and on various spatial emission is not a good indicator of cold gas in scales, information was still missing on the cold NGC4151, or that the relatively low column density gas in between the leading side of the large scale in this X-ray dominated region leads to a low CO stellar bar (at about 1 kpc from the nucleus) and the abundance relative to H₂. The upper limit of the cold putative torus observed in HI absorption on parsec molecular gas mass from the CO line in the central scales. 300pc is 10⁵ M, which is sufficient to support the AGN activity at its current levels for 10⁷ yrs, the Using the Plateau de Bure interferometer, Dumas typical lifetime of nuclear activity. and collaborators obtained the first spatially resolved spectroscopic imaging observations of the ¹²CO(1-0) line emission in the central 2.5kpc of NGC4151. COLD GASS - an IRAM Legacy The 3mm continuum emission was found to arise Database for the GASS from the location of the active nucleus with a Survey flux of 14mJy and appears to be unresolved at an angular scale of about 2.8” (or 180pc). The total cold One of the most fascinating aspects of galaxies in molecular gas mass detected is 2,107 Msun. Most of the local universe is the complex system of correla the CO is distributed along two curved features, tions between their global physical properties. These about 1 kpc north and south of the active nucleus correlations form the basis of the so-called scaling and coincident with the circum-nuclear dust ring. laws, which are important because they provide The gas kinematics within these arcs is consistent quantitative means to understand the physics of with motions due to the large-scale stellar bar, galaxies, their formation and their evolutionary his derived from neutral hydrogen observations. Two tory. Scaling laws have been proposed for a variety of properties and systems, but only very few exist Moment maps of the ¹²CO (1- that describe how the global cold gas properties 0) line emission in NGC 4151: integrated intensity (top), correlate with other global physical properties of velocity field (middle), and velocity dispersion (bottom). galaxies. To shed new light on how the cold gas, The cross marks the location of the active galactic nucleus. atomic gas and stars relate to each other, Kauffmann and Kramer initiated with their collaborators the From Dumas et al. 2010, ApJ, 721, 911 COLD GASS observational project. COLD GASS is an international collaboration and an ongoing 30-meter telescope Legacy Survey using EMIR, that is aimed at measuring the amount of cold gas through the ¹²CO J=1-0 emission line in a statistically representative sample of massive (M*>10¹⁰ M) galaxies in the local Universe (0.025 The figure shown herewith displays first results of the survey. The left-hand panel shows the relation between the molecular gas fraction M(H₂)/M* and the NUV-r color of a sample of 222 galaxies. It appears that the empirical threshold of NUV-r=5 Annual report 2010 11 marks an abrupt transition from the active gas-rich coverage and angular resolution of this map allows a star forming galaxy population to a more passive comparison of the distribution and the dynamics of population characterized by molecular gas fractions the molecular gas with maps at other wavelengths lower than 0.015. with comparable spatial coverage and resolution as shown in the accompanying figure. The date displayed in the right panel indicates that the mean molecular gas depletion time scale In the southwest region of the nebula, Berné et al. increases by a factor of 6 across the mass range reported the presence of a series of regular waves sampled by the NUV-r<5 galaxies of the COLD (ripples) enshrouding an elongated molecular GASS survey, and that this variation correlates cloud and displaying strong velocity gradients. This strongly with specific star formation rate, NUV-r structure follows closely (with clear stratifications) color and stellar mass. Previous surveys were unable similar features that are traced in H₂ and in the to observe this variation because of the limited emission features of very small grains (PAHs). From statistical range of their samples. While it is known a careful analysis of the relative distribution of that gas depletion times are significantly shorter in these various tracers, the authors conclude that this starburst galaxies and mergers of the local Universe, remarkable periodic structure and its velocity field the importance of these results is two-fold. First, they are consistent with hydrodynamical instabilities that produce compelling evidence that the gas depletion result from the interaction of high-velocity plasma/ timescales also varies within the population of gas, produced by massive stars, with the dense “normal” star-forming galaxies, and, second, these molecular gas. The characteristics of the structure results quantify this variation as a function of a range are consistent with a Kelvin-Helmholtz instability of fundamental parameters. that arises during the expansion of the nebula as gas heated and ionized by massive stars is blown over pre-existing molecular gas. A new instability revealed in the Orion molecular cloud Fragmentation and mass Massive stars influence their immediate surrounding segregation in Cygnus X and have profound impacts on their parental mole cular clouds, fragmenting, compressing and disrup Massive dense cores (MDCs) are the high-mass ting them. Hydrodynamical instabilities are thought equivalent of the so-called dense cores in nearby to play a fundamental role in these processes star-forming regions. With typical sizes of 0.1 pc, although identifying them remains difficult. The they could form either a few high-mass stars, or Orion nebula is the closest-by example of a region a cluster of low-mass stars. To constrain the result forming massive stars (at a distance of 414 pc) and of the fragmentation process in regions that offer has therefore been a choice laboratory for exploring the opportunity to reach scales at which individual the influence of massive stars on the surrounding collapsing objects can be separated, Bontemps and molecular gas. Recently, Berné and collaborators collaborators observed the six most massive and have obtained a new complete map of the Orion youngest dense cores in the Cygnus X complex nebula in ¹²CO(2-1) using HERA at the 30-meter using the Plateau de Bure Interferometer at 1.3 and telescope with a spatial resolution of 12” (0.025 pc) 3.5 mm. and a spectral resolution of 0.4 km.s-¹.The spatial First results of the COLD GASS project (Left panel) Molecular gas mass fraction as a function of NUV-r color for the actual COLD GLASS sample. Secure detections are represented as filled circles, tentative detections as open circles, and non-detections are indicated by arrows. (Right panel) The depletion time - specific star formation rate relation at z=0, 1 and 2, for normal and extreme star forming galaxies. From Saintonge et al. 2011, MNRAS, 415, 32 & 61 12 Institut de Radioastronomie Milimétrique in the protostellar fragments are also indicative of an enhanced efficiency of core formation in the MDC. The increase in the core formation efficiency as a function of average density in the MDCs is suggested to be due to the increasing importance of self-gravity that leads to gravitational collapse on the scale of the MDCs. At the same time, the observed MDCs tend to fragment into a few proto-stellar objects within their central regions. Bontemps et al. conclude that we are probably witnessing the primordial mass segregation of clusters. The Protoplanetary Disk around the Young Star LkCa15 Hundreds of exoplanets have been discovered around nearby main-sequence stars. A massive effort is underway to find more planets, determine With the exception of the most compact MDC their key properties, and explain demographic Multiwavelength overview of (CygX-N40), which harbors a single protostellar trends with models of their formation. But asso the Orion nebula. a) Spitzer object of ~60 M, the remaining MDCs seem to have ciating the current exoplanet properties with their mid-infrared image of the Orion nebula. b) Overlay of collapsed into a number of compact fragments with formation epoch can be problematic, since the the IRAM 30-meter ¹²CO J=2-1 sizes and separations similar to low-mass pre-stellar formation process is intimately associated with the maps integrated emission condensations and Class 0 young stellar objects in initial conditions in the progenitor circumstellar disk. in velocity between -5 and 8 (blue), and 12 and 25 km.s nearby proto-clusters. The level of fragmentation Ideally, the properties of mature exoplanet systems -1 (red), tracing the cold is found to be higher than in the turbulence could be compared with those for their younger (10-100 K) molecular gas, regulated monolithic collapse scenario but not as counterparts that are “caught in the act” of formation, and 8 μm emission from the Midcourse Space Experiment high as expected in a pure gravo-turbulent scenario still embedded in their natal disks. The results (MSX) (green) tracing dust where the distribution of mass is dominated by would refine our understanding of planet formation and warm (~100-1000 K) gas low-mass (proto)stars. The high fractions of mass timescales and help characterize how exoplanet at the surface of clouds. c) The series of images show the ripples seen in ¹²CO (2-1) emission at different velocities overlaid on the Spitzer 3.6 μm map (green) attributed to small grains (PAH). In panels a and b, the white solid contours show the delimitation of diffuse soft X-ray emission tracing the hot plasma detected in the X-rays. From Berné et al. 2010, Nature 466, 947 CygX-N48 (top) and CygX-N53 (bottom) are two MDCs located in the filament of DR21. Both reveal a complex and extended structure at 3.5mm (left) with one or two main cores in the central regions that divide into smaller fragments at 1.3mm (right). From Bontemps et al. 2010, A&A, 524, 18 Annual report 2010 13 properties are shaped by early interactions with disk the dense, dusty layers of the envelope inducing material. shocks and structural deformation. While the direct detection of a planet orbiting a In the frame of the COSAS (CO Survey of late AGB young star is currently a challenge, the presence of Stars) collaboration, Castro-Carrizo and collaborators a giant planet can be inferred indirectly through its have mapped and analyzed the ¹²CO J = 1-0 and dynamical influence on the structure of the remnant 2-1 emission lines in a representative sample of disk material. A sufficiently massive planetary circumstellar envelopes around AGB and post-AGB companion can open a gap that impedes the inward stars. The survey was undertaken with the aim of flow of mass through the disk, quickly producing investigating small and large-scale morphological a low-density cavity at the disk center. The size of and kinematical properties of the molecular environ the cavity is set by the planet orbit, and the amount ment surrounding stars in the late AGB and early of material inside it depends in some way on the post-AGB phases. For this, COSAS combines the high planet mass. Therefore, observational constraints sensitivity and spatial resolving power of the Plateau on the sizes and mass contents of these disk cavities de Bure interferometer with the better capability of can offer some initial insights into the orbital the 30-meter telescope to map extended emission. architectures and masses, respectively, of planetary The global sample encompasses 45 stars selected systems at ages of only ~1 Myr. The best way to to span a range in chemical type, variability type, measure such disk structures is with high-quality, evolutionary state, and initial mass. COSAS provides sensitive, and high angular resolution observations sensitive means to quantify variations in the mass- of the millimeter dust continuum emission. loss rates, assess morphological and kinematical features, and investigate the appearance of fast Using the new band 4 receivers and the WideX aspherical winds in the early post-AGB phase. correlator in the A configuration, the Plateau de Bure interferometer has recently resolved the Based on this survey data, the authors conclude large cavity (R = 50 AU) in the proto-planetary disk that the envelopes around late AGB stars are around the young star LkCa15 at a continuum mostly spherical, often mingled with features such frequency of 346 GHz. While a detailed modeling as concentric arcs (R Cas and TX Cam), broken effort will be required to interpret the properties and spiral density pattern (TX Cam), molecular patches underlying origins of this cavity, these exceptional testifying to aspherical mass-loss (WX Psc, IK Tau, V data represent a first step in the development of a Cyg, and S Cep), as well as with well-defined axis- new, indirect method for identifying potential young symmetric morphologies and kinematical patterns exoplanet systems through the sub/millimeter (X Her and RX Boo). The COSAS sources span a wide imaging of their associated disk structures. range of angular sizes, from relatively compact (CRL 2362, OH 104.9+2.4 and CRL 2477) to very large (χ Cyg and TX Cam) envelopes, sometimes partially obscured by self-absorption features, which testify to the emergence of aspherical winds in the inner-most The COSAS Survey of AGB circumstellar regions. and Post-AGB Stars The evolution of transition objects between the asymptotic giant branch (AGB) and the planetary Image of the 346 GHz nebula (PN) phase is spectacular, probably the dust continuum emission from the LkCa 15 disk all-decisive moment where very efficient mass measured with the Plateau loss processes determine the basic morphological, de Bure interferometer in A-configuration. The 0.39” dynamical and chemical layout of the future PN. x 0.18” synthesized beam is shown in the lower left, with a While these processes are not well understood, 40 AU scale bar labeled to the lower right for reference. This radiation pressure on dust grains in the cool and is the highest spatial dense circumstellar shells and atmospheric shock resolution image obtained with the Plateau de Bure waves driven by inner envelope pulsations are both Interferometer. suspected to be at work. According to present From Andrews et al. (2011) knowledge, the rapid evolution of stars towards in preparation the end of the AGB seems to be related to the appearance of high-velocity winds in the innermost regions and a clear breakdown of the spherical symmetry of the circumstellar envelopes. These winds, which are often highly collimated, run into 14 Institut de Radioastronomie Milimétrique First observations of therefore expected. Yet, remarkably, Agundez and interstellar anion CN- collaborators succeeded in detecting 3 lines in the millimeter wave spectrum of IRC+10216 that they The discovery of interstellar anions is probably could assign to CN-, the shortest of the two anions. the most remarkable result recently obtained in the field of astrochemistry. After the synthesis The three lines are shown in the accompanying - - - - and characterization of C₄H , C6H , C8H and C3N in figure. The first two lines (one appears as a low the Harvard spectroscopic laboratory and their intensity shoulder of a much stronger C6H line, the subsequent identification in the spectrum of other as a broad feature blended with a SiC2 line) IRC+10216, a fifth anion was identified in 2008 in the were tentatively assigned to the J=1-0 and 2-1 same source without the help of any laboratory data: transitions of CN- but only the detection of the J=3-2 - - C5N . Up to now, only the n=1 members of the C2nH transition using EMIR (shown in the upper panel) - and C2n-1N series remained unidentified in space, ultimately led to the clear-cut and unambiguous although their transition frequencies are precisely identification of the anion: its rest frequency, which known. was found identical to the predicted one, left little doubt on the detection of CN-. C-chain anions are believed to be formed by electron radiative attachment on neutrals. As The abundance of CN- derived from the line - predicted by models, the abundances of C6H and intensities is many orders of magnitude larger - C8H are fairly large and represent a good fraction than predicted by statistical theory calculations of (~1/10) of the abundances of their parent neutral electron attachment. Although electron attachment species C6H and C8H. On the other hand, the rate coefficients are difficult to calculate precisely - abundances of C4H and C3N- relative to C4H and and are only evaluated through statistical theory, the C3N are much smaller (≤1/4000). This is explained disagreement seems much too large and suggests ¹²CO J=1-0 and 2-1 line maps by the fact that C H- and C N- are shorter than C H- another formation route than the attachment of an at the systemic velocity of 4 3 6 - a selected sample of AGB and C8H and have less low-lying vibrational states, electron to CN. and post-AGB stars from the COSAS survey. making electron attachment less probable. For the From Castro-Carrizo et al. 2010, very short radicals CN and C2H, which have only a A&A, 523, 59 few vibrational states, the theory predicts vanishingly small electron attachment rates. The non-detection - - of CN and C2H , down to very low levels, was Annual report 2010 15 Spectra of IRC+20216 Zooming in on the Nucleus covering the J=1-0, 2-1 and of Comet 8P/Tuttle 3-2 transitions of CN-. Grey boxes mark their expected positions based on Comets have challenged generations of laboratory measurements. astronomers, yet much remains to be understood From Agundez et al. 2010, about the properties of their nuclei. Understanding A&A, 517, L2 their physical and chemical properties is one of the most challenging issues in the study of planetary formation. They potentially provide crucial details on the initial thermo-physical conditions of the Solar proto-planetary disk and on the subsequent formation of the icy planetesimals from which the cores of the outer planets were formed. During a recent observing campaign using the Plateau de Bure interferometer, Boissier and collaborators succeeded in observing the thermal continuum emission at millimeter wavelengths from the nucleus of Comet 8P/Tuttle. It was ejected to the outer Solar System and preserved in the Oort cloud until it came back in the inner Solar System as a Halley type comet. Observed at 240 GHz on January 8, 2008, it was detected with a flux density of ~3 mJy. By combining these millimeter measurements with visible and mid-IR data, the authors were able to constrain the surface properties of the ~2.5 km-sized nucleus and derived a thermal inertia ≤10 J/K.m-2.s-1/2 and a millimetric emissivity of ~0.7-0.8. This low emissivity suggests the sub-surface layers of the nucleus do contribute to the detected continuum emission. Synthetic thermal light curve of Comet 8P/Tuttle, phased relatively to the radar observations of Harmon et al. (2010). The shape model is from HST observations by Lamy et al. (2008, 2010b). The thick solid line corresponds to the time interval of the Plateau de Bure observations. From Boissier et al. 2011, A&A, 528, 54 16 Institut de Radioastronomie Milimétrique Pico Veleta observatory Data subset of EMIR spectra Several important events took place at the 30-meter described below was focused on preparing for yet at 0.85mm of the O-rich stars telescope on Pico Valeta, including the installation larger bandwidths to be covered by fast Fourier IK Tau and OH231.8+4.2, which are part of an on-going of the new Fourier transform spectrometers, the transform spectrometers. mm-wavelength spectral replacement of the gearboxes and the successful line survey of O-rich evolved testing of new bolometer cameras. During the winter semester 2010/2011, the fast stars. Bottom: Selected spectra obtained with WILMA Fourier transform spectrometers (FTS) were around 300 and 343GHz. As in previous years, the 30-meter telescope is offered for the first time for routine observations. The The molecular species highly demanded by the community with almost available eight FTS units cover 8 GHz of bandwidth responsible for some of the at 195kHz resolution. These units only form the first most intense transitions 200 projects that were observed during 2010. detected are labeled. Top: About an equal number of observers visited the part of the extension to 24 units, which is planned Zoom of a smaller frequency observatory to conduct their own observations for autumn 2011. This revised IF system will cover range (indicated by vertical an instantaneous bandwidth of 32GHz. In order dashed lines in the bottom or help with other projects during several weeks panels) showing higher of pooled observations. The new eight-mixer to prepare for this major upgrade, we started to spectral resolution spectra receiver EMIR, including its new 345 GHz band, revise the entire data handling system of hard- and obtained with FTS. (Work software (see below). by Sanchez Contreras and is strongly demanded due to its unique sensitivy collaborators) and bandwidth. A large part of the technical work Since December 1, 2010, the 8 GHz FTS have been successfully used with EMIR in all observing modes. An example of data obtained with this new facility is displayed hereby and demonstrates the power of the new system. It shows frequency surveys near 346 GHz using the WILMA and FTS backends of two Oxygen-rich circumstellar envelopes around evolved stars that both show a wealth of emission lines witnessing the chemical complexity. Two prototype bolometer cameras were tested at the telescope in 2010. The GISMO 2mm camera has 128 pixels and uses transition edge sensors (TES) and squid amplifiers and multiplexers for readout. In April 2010, the GISMO team, led by Johannes Staguhn (Goddard/USA), tested a much-improved instrument in a 3rd test run at the 30-meter telescope. Remaining problems were identified. With the help Annual report 2010 17 of the CRUSH-2 data reduction package written by A. Two global 3mm VLBI sessions were carried out Kovacs some very promising results were obtained. during 10 days in 2010. A dedicated test at 1mm For example, the starburst galaxy AzTEC-3 at a between the Pico and the Plateau de Bure showed redshift of z=5.3 was detected with a flux density of good quality fringes. 3.7mJy at 2 mm (Capak et al. 2011). The Neel IRAM KIDs Array (NIKA) camera uses TELESCOPE OPERATION kinetic inductance detectors (KIDs). For the 2nd test run at the 30-meter telescope in October 2010, About 60% of the total time in 2010 was used for the instrument had been upgraded to include observations and about 30% of the time was lost dual-band optics for simultaneous observations due to adverse meteorological conditions. The at 150 and 220 GHz using two spatially separated amount of time lost is much less during summer KID arrays. In this version of the instrument, a grid than during winter, similar as in previous years. polarizer achieves the band splitting. The arrays About 10% of the time was used for regular comprised 144 pixels at 2mm and 256 pixels at maintenance and dedicated technical projects. Less 1mm. A number of faint and extended objects were than 0.8% of the time (about 68 hours) was lost due imaged including SgrB2, Cygnus A, and NGC1068 to technical problems. Here, we only count failures of (Monfardini, Benoit et al. 2011). more than 2 hours, which are directly noticed by the staff. However, each important failure is monitored, analyzed and discussed to further improve the ASTRONOMICAL PROJECTS system. During the year 2010, a total of 188 projects were Out of the 68 hours, 28 hours in total were lost in the scheduled at the 30-meter telescope. This number telescope area, 16 hours were lost due to front-end includes 3 Large Programs, 14 Director’s time problems, and about 24 hours because of computer proposals (DDT), and 8 VLBI projects. A large fraction related problems. of these projects (74 or 39%) was scheduled in pools. The fraction of projects observed remotely has Time distribution at the IRAM increased further, to 11% (20 projects). 30-meter telescope in 2010 192 observers visited the observatory during the reporting period. Many of these visitors came two or more times to the telescope. Forty observers came to help with the pool observations, and seven of them actually came for more than one week. From the proposals eligible for RadioNet support, 27 were scheduled at the telescope and 8 European observers were granted travel support. Monthly time distribution at the IRAM 30-meter telescope (U.Observ.: Observations, U.T.T.: technical tests, U.Mainten.: Maintenance, S.Wind: Stopped because of high wind velocities, S:Meteo: Stopped because of other meteorological conditions, S:Techn.: Stopped because of technical problems). Monthly time distribution at the IRAM 30-meter telescope (U.Observ.: Observations, U.T.T.: technical tests, U.Mainten.: Maintenance, S.Wind: Stopped because of high wind velocities, S:Meteo: Stopped because of other meteorological conditions, S:Techn.: Stopped because of technical problems). 18 Institut de Radioastronomie Milimétrique old gearboxes exhibited enhanced vibrations indicating wear. In preparation of this exchange, we characterized these vibrations and installed two new electrical cranes to permit moving of up to 3 tons inside the antenna tower. We also installed manual cranes in the roof of the motors room, which had to be reinforced. The gearboxes were characterized by measuring stiffness, transfer function, hysteresis, rolling friction, operation of brakes, etc.. The exchange went very well and smoothly due to a careful preparation. It is planned to replace the remaining 4 gearboxes in 2011 and 2012. ■■ In early 2010, a protective plate of one of the legs was blown off the 30-meter telescope. It was replaced during the summer period. To prevent such problems in the future, the rivets of the back- structure were revised. Several tens of rivets, that New Azimuth gearbox being craned into the motors room of the 30-meter telescop New Azimuth gearbox being showed signs of wear, were replaced. craned into the motors room of the 30-meter telescope ANTENNA AND ELECTRONICS ■■ The telescope sun avoidance system was improved by implementing a mechanism to The main effort and activities in the telescope automatically close the antenna vertex when the area were related with the daily operation of the distance between the antenna beam and the observatory: periodically maintaining the systems sun is less than 0.75°, i.e. in case the antenna has and equipments for observation, including the accidentally moved into the sun avoidance zone pointing model, helping with the daily problems of 1°. This mechanism is independent to what is concerning the observation and operation, and implemented in the antenna control program repairing broken equipment. ‘AntennaMountDrive’ and works all the time, even when the antenna is stopped. The main goal is to Other activities in the telescope area during 2010 protect the receivers from being saturated. that deserve to be mentioned are: ■■ The antenna Error Beam was measured with Moon Motors room of the 30-meter observations in collaboration with A. Greve and C. telescope with original ■■ gearboxes During two weeks in September 2010, two Kramer. New values of the Error Beam improve on of the six antenna gearboxes were replaced, the findings of 1998. A report is in preparation. one for azimuth and one for elevation, by new ■■ Measurements were done to characterize gearboxes built by the German company Desch. the antenna gain elevation curve, telescope This exchange became necessary as some of the efficiencies, and insertion losses of the vertex radome at 340 GHz. FRONT-ENDS The EMIR receiver continues to produce data of exceptional quality and, by now, can be considered to be the core of the 30-meter telescope front- end area. Acquired experience over the past two years show new effects that were not detected during the initial commissioning phase. Some new interferences at fixed frequencies in the IF band were found. Whereas some of these spurious signals are from a known origin (oscillators from other receivers), others are not yet understood and are still under investigation. A mechanical problem on one of the EMIR calibration motors stopped receiver operation during some days. One of the position sensors was found defective, probably due to the very frequent use of the part. The damaged piece was replaced but a longer-term solution needs to be found. Annual report 2010 19 The IF system will be upgraded to a total bandwidth of 32 GHz in 2011, doubling the bandwidth available for the backends. To prepare for the strong increase in the total instantaneous bandwidth, a revision of the IF transport and switching scheme has been started. A new equalizer unit, good for 4 new coaxial cables, each transporting 4 GHz of bandwidth, was built. The EMIR receiver will be upgraded further in 2011 by installing 2SB mixers for the E230 and E330 bands. Some performance degradation was found on one of the HERA Local Oscillator (LO) boxes. The two oscillators were completely refurbished in Grenoble and later installed and commissioned at the telescope. Tests on experimental bolometer cameras (GISMO HEMT test receiver at the 30-meter telescope. and NIKA) were continued over the year. The In preparation of the new IF system, which will offer HEMT test receiver at the bolometer prototypes include new upgraded 32GHz of instantaneous bandwidth with 24 FTS 30-meter telescope. sensors arrays providing a much-improved sensitivity units, we installed a second distribution box for 4 (see above). more IF cables transporting 4GHz each. Finally, a new dual polarization HEMT test receiver Work on new broadband continuum detectors was installed in August 2010. Initial results, after continued in 2010. The temperature control, detec commissioning at the telescope, show very close tor boards, data readout, and the FPGA program agreement to measurements made in laboratory ming were developed for commissioning in spring conditions in Grenoble. The results are also com 2011. parable in performance to the best SIS receivers. Allan variance results demonstrate good receiver For the VESPA auto-correlator spectrometer, offset stability, even comparable to the specifications for voltage corrections were installed for all samplers to ALMA receivers. This fact, coupled to the extremely adapt to the increased dynamic range between the large bandwidth (>30 GHz), makes this receiver a cold load and the sky of EMIR. good candidate for pointing and other continuum measurements. The prototype receiver will help in solving the question of which technology to use for COMPUTERS a future 3 mm multi-beam heterodyne array. In the computer group, the following activities took place in 2010. BACKENDS ■■ New Server System at the Observatory: The In autumn 2010, 8 new fast Fourier transform server computers that control the telescope that spectrometers (FTS) from Radiometer Physics are used for data-processing (mrt-lx1,..,3) were (Meckenheim, Germany) were integrated into the replaced. The new computers are equipped with system. This FTS will enable observations with EMIR, faster processors, more cores and more memory. using the 2x4GHz bandwidth with a resolution of Each computer now has 16 disk slots, which allows 195 kHz. The FTS units were connected to the 4 MHz installing up to 96 TB of disk space (based on 2TB processor and installed in parallel to the 4 MHz disks). A fallback hardware (mrt-lx0) is available to backend. In preparation, the synchronization signals replace a broken server. In order to prevent disk had to be debugged with help by Bernd Klein failures, all system have a RAID controller installed at the MPIfR (Bonn, Germany). Data transfer and with hot-swap spare disks. control were developed and a new 19” rack for the IF processor and three FTS crates were installed in the ■■ A tape autoloader that can automatically load backend room. Since the start of the winter semester one LTO tape from 16 tapes was installed and 2010/2011, the FTS units have been successfully the LTO-5 tapes that have a capacity of 1.6TB offered to the astronomers and first results are (uncompressed) were switched. The backup sys displayed above. tem was changed to use the open-source tool ‘Bacula’. 20 Institut de Radioastronomie Milimétrique ■■ Moving from 32 to 64 bit systems: During the of the 30-meter telescope to its limits. These preparation for the new FTS back-ends, it was improvements are now also active for standard realized that the current operating system observations, including the execution of scans and (32-bit architecture) imposed a severe limit on alarms for tracking problems, with simple default data reduction. When the hardware of the main values, though some fine-tuning remains to be telescope control and data reduction computers done. was updated, it was decided to also change the system architecture to 64-bit. This implied a new Unification in the NCS software development operating system. The basic architecture is now was achieved allowing the observer to use the 64-bit, but support for programs compiled for 32- same revision of paKo and the same version of bit architecture was also installed. the antenna mount drive software for routine observations using the heterodyne receivers, ■■ Telescope Control: Today the telescope control MAMBO, and GISMO. system supports the new FTS backends. The increase in backend channels (approx. 10 times Before and after the gearbox exchange, all the more) requested the replacement of the server tracking and observing modes were extensively systems at the observatory as described above. tested to assure the tracking quality. ■■ The receiver control software was modified to At the less “visible” levels, improvements were made support the HEMT receiver installed in 2010. A in the limits for the EMIR frequencies, in several alarm new fallback hardware for the MAMBO backend and warning messages, antenna tracking, secondary (ABBA) has been installed. (“spindles”) control, sun avoidance, support for experimental instruments, e.g., the HEMT receiver ■■ Organization of observing projects: The project and the NIKA bolometer, and other aspects of the organization has been improved. Projects and NCS. TAPAS accounts are now created based on the information from the IRAM Scheduler database. The Principal Investigator is informed by e-mail MISCeLLANEOUS that the project has been created and can be accessed via Internet. In April 2010, Breezy Ocana, finished her PhD thesis on “The interstellar medium in nearby elliptical ■■ TAPAS database of observations header radio galaxies” and successfully defended it at the information: The data-format of the observation Universidad de Granada. Jorge Abreu Vicente, who header information for the CDS (Centre de graduated at the Universidad de La Laguna on Données astronomiques de Strasbourg) has been Tenerife, joined the team of astronomers in Granada defined and a first set of data included into the in August, and became a new Astronomer of Duty CDS database (2009-10/12). and PhD student. End of July, Helmut Wiesemeyer left IRAM for a sabbatical year in the group of Karl CONTROL SYSTEM (NCS) Menten at the MPIfR (Bonn, Germany). Albrecht Sievers has taken over Helmut Wiesemeyer’s work of The main effort in the development of the NCS maintaining and developing the calibration package in 2010 was the support of the new FTS backend. MIRA and the online data processing (odp), and This includes the beginning of a major revision of preparing for the new high resolution Fast Fourier the logistics of the data handling and processing Transform Spectrometers. because of the much larger data rates. As in previous years, IRAM offered guided tours More technical time than usual was lost to bad through the observatory and public talks to a weather, creating a bottleneck in NCS testing, broader public during the summer months. These particularly toward the end of 2010 – without outreach activities were organized in collaboration harming the observations except that we needed with the Instituto de Astrofisica de Andalucia (IAA). to schedule some additional Technical Time in December. Moreover, several developments started in 2010, remained unfinished. Further improvements were made of the safeguards for the experimental observing modes for GISMO, i.e. Lissajous curves, which use the tracking capabilities Annual report 2010 21 Plateau de Bure observatory The operation of the Plateau de Bure Interferometer science demonstration programs was observed that in 2010 has been as exciting as in previous years, gave a first glimpse of the exciting new observing characterised by outstanding scientific results and a possibilities the new band was opening up. First number of major technical achievements. images from the commissioning and science demonstration phase revealed the power of the A first technical breakthrough was achieved in interferometer (see Science Section) and helped the spring: WideX, a broadband correlator with to identify areas where work had to be done to 3.6 GHz frequency coverage in each polarization, a improve operational reliability. The performance of channel spacing of 2 MHz, and a modular design to the Band 4 system has met our highest expectations. support an array extension to 8 antennas, went into By opening the new band to astronomical research, operation after several weeks of intensive testing. it has now become possible to observe with a The new correlator, which is operated in parallel to spatial resolution of ~0.2” in the most extended the narrow-band correlator, is working well since configuration of the interferometer, and with then and shows excellent performance. unprecedented details when observations are made with the instantaneous sensitivity of the broad The next highlight was reached at the end of the band correlator. Regular user-requested Band 4 year when Band 4 (275 to 373 GHz) was opened to observations have been scheduled and successfully the astronomical community. The full integration obtained since the beginning of 2011. of the ~100 GHz wide band called for a number of system upgrades among which the most signifi While much of the focus at the Plateau de Bure cant were: the installation of the remaining eight Interferometer has been on Band 4 and the new Band 4 mixers (two antennas were already equipped correlator, the project to develop and implement in 2009), a complete refurbishment of the local additional logic to provide full-Stokes polarization oscillator transport system, a major modification imaging capabilities to the system has also been of the system control software and a thorough making progress in 2010. A digital switching refitting of the data acquisition software. After circuit was implemented that interconnects the months of preparatory work, three weeks during polarization IF bandsplitters of different antennas to which the array was not available for astronomical compute all possible parallel- and crossed-handed observations, and a few days of testing at the correlation products. The project, which is being beginning of December, the instrument com carried out in collaboration with the Observatoire missioning team reported the successful measure de Bordeaux, generated a first scientific result, which ment of interferometric fringes using Band 4. The provided a first proof of concept for a possible commissioning was carried out in two phases: after implementation of a polarimetric observing mode a short technical validation of the instrumental for users of the Plateau de Bure Interferometer. performance over the Christmas period, a series of 22 Institut de Radioastronomie Milimétrique OBSERVATIONS 170 different projects, including 4 Large Programs and 21 proposals for Director’s Discretionary time, The interferometer performed according to corresponding to 112 different observing programs, expectations with almost no downtime due to were scheduled at the Observatory in 2010. As in hardware upgrades. The receivers and the antennas previous years, the weight on extragalactic research all worked well throughout the year. Observations remains considerable with about twice as many were done in periods of excellent phase stability proposals submitted than in the field of young stellar and atmospheric transparency at the beginning and objects. Also, a large amount of observing time at the end of 2010, and faced rather unseasonable was invested in D-configuration between spring conditions in spring. The excellent weather con and fall in the detection of line-emission (mostly of carbon monoxide) in galaxies at high redshift. The second week in May and October was devoted to coordinated 3mm VLBI continuum observations with several participating radio observatories in Europe and the United States. Annex I details all the proposals to which time was granted in the course of the year, and the great number of papers, that were published in 2010 and are based on data obtained at the interferometer, testifies to the high scientific return of the Plateau de Bure Interferometer. Plateau de Bure observing time and atmospheric water ditions at the end of the year were used for the ANTENNA SURFACE vapor statistics over the last ten years. The overall commissioning and science verification of Band 4. IMPROVEMENTS correlation time accounts for 50% of the total time The move to the A configuration was deferred to in the year 2010. Band 3 January 5, 2011, and was so accomplished about In the context of the antenna surface refurbishment (200 – 274 GHz) and Band 4 (275 – 373 GHz) programs two weeks later than in the winter 2009/2010. As in project (which started in 2007), a special effort and observations in the most extended (AB) configurations previous years, the scheduling of the A configuration was made in the antenna maintenance period to are for the most part carried was readjusted shortly after the beginning of the resurface the remaining two antennas and thereby out in the winter months. winter scheduling period to optimize the observing resolve the issues related to panel degradation and of A-rated projects with respect to Sun avoidance antenna efficiency losses. Surface refurbishment limitations and weather constraints. As of February work started on antenna 1 in the first June week 8, 2011, 41 A-configuration tracks, corresponding to and was completed on July 3, 2010. On antenna 6, 22 astronomical programs and 6 Band 4 programs, work started around the middle of September and were observed with remarkable sensitivity and was completed at the end on October 16, 2010. successfully completed. As in previous years, the carbon fibre panels were replaced with new precision-machined aluminium As in previous years, the percentage of telescope panels (by MECACHROME) using a chessboard contiguous correlation time scheduled for observing like technique to reduce the number of iterations programs was on average 50% percent of the total required in the process of achieving highest surface time. Additional 20 percent have to be accounted for precision. In a subsequent series of holographic receiver tuning, testing equipment, surface adjust surface measurements final surface precisions of ments and antenna maintenance, and on complet 45μm (not weighted by illumination) and 46μm ing the commissioning and science verification of were achieved for antenna 1 and 6, respectively. WideX, the new LO transport system and band 4; the remaining 30% were lost because of precipitation, As in previous years, the surface quality of all the wind and inadequate atmospheric phase stability. antennas was verified by means of holographic measurements at the end of the maintenance The Program Committee met twice during the year, period. Surface panels were readjusted when around four weeks after the deadlines for submission deemed necessary. of proposals and reviewed 220 applications. The April meeting was seriously disrupted due to travel In connection with the plans to compensate difficulties resulting from the Icelandic volcano for the central gravity sag of ring 1 panels, a eruption. As a result the Program Committee met fourth mechanical point was added on antenna for the very first time via telephone conference to 4 to support the center of the panels and the Grenoble from their home institutes. More than achievable surface quality improvement assessed Annual report 2010 23 by holographic measurements. The support points ANTENNA STATIONS were installed during the maintenance period 2009 but the final positional adjustments were only made Accurate knowledge of the antenna positions is of in early 2010. A semi-quantitative assessment of paramount importance to adequately compensate the panels’ stability, obtained over the last months, for the geometrical delay. In 2009, the inclination suggests that the additional support point is angles of the azimuth axis of some of the antennas instrumental in ensuring the panels mechanical were found to change significantly over a period stability and containing the antenna efficiency of several weeks. Detailed investigations revealed losses. Based on this assessment, it is planned to that the changes in the antenna inclination appear equip the remaining five antennas with a fourth to be linked to positional instabilities of the station mechanical point in the maintenance period 2011. on which the antennas are clamped, and that these changes occur more often in the spring, when Aperture phase patterns of antenna 1 (left) and 6 (right), respectively after the surface refurbishment. A series of warming conditions bring melting snow and heavy holographic surface measurements was needed to readjust the precipitation. To remedy this problem, the antenna primary surface of the refurbished antennas to a precision of 45μm rms (left) and 46μm rms (right). Contours are given in steps inclination is now monitored over time to ensure the of 100μm. best possible relative antenna positions at any time. ANTENNA SUN AVOIDANCE In the context of the antenna primary surface refurbishment plan, Sun illumination measurements were started in 2008 to investigate the possibility of relaxing the initial Sun avoidance constraints (45 deg). The results of these investigations led to the design of a new Sun sensor that will permit observations down to a Sun distance of 25 deg. A first step was made in 2009 with the old sensors by reducing the Sun avoidance circle to 35 deg, and a second was planned for 2010 with the new sensors by reducing it further down to 25 deg. By relaxing the Sun avoidance constraints from 45 deg to 25 deg, the region of the sky inaccessible to observations on any given date will become less than 5%, and will make many more objects of the sky accessible to observations in the extended configurations of the array. Due to the exceptionally heavy schedule of activities at the Observatory during the summer maintenance period 2010, the decision was made to limit the installation of the Sun sensors to only one antenna and to defer the installation of the remaining sensors to the antenna maintenance period 2011. RECEIVER BAND 4 AND LO TRANSPORT SYSTEM The strong astigmatism-like deformation detected on antenna 3 in the summer 2009, and repeatedly Significant efforts were made in the context of observed over the winter period 2009/2010, the project to equip the antennas with the Band was found to be unrelated to deformations of 4 (275 – 373 GHz) receiving system: 1) the ageing the secondary mirror. The deformation having HP synthesizers were replaced each with Rohde disappeared without any apparent reason in the & Schwarz frequency generators to meet the spring 2010, a physical origin for the deformation tight constraints on phase stability, 2) the Local could neither be identified, nor be demonstrated. Oscillator transport system was refurbished to a) accommodate a pair of diplexers (one for each reference) to transport the phasing references (0.5 24 Institut de Radioastronomie Milimétrique MHz and 100 MHz) and the generator frequency in which a project is observed in order to keep some (1600-2000MHz) over a single coaxial cable, and pieces of information confidential until that time. b) replace the out-dated, mechanically driven LO1 reference signals with YIG voltage controlled oscillators that feature broadband operation SEVENTH SCHOOL ON (13.2-16.4 GHz) and a much better phase noise MILLIMETER INTERFEROMETRY performance, 3) the LO1 boxes of Bands 1-3 were modified to match the new reference signals, and The Seventh IRAM Millimeter Interferometry the antennas all equipped with band 4 LO1 boxes, School took place from October 4 to 8, 2010, at 4) the receivers of the remaining 4 antennas were the IRAM headquarters in Grenoble. The school finally fit up with 2SB ALMA-type Band 4 mixers focused on both theoretical and observational operated SSB. aspects of millimeter interferometry. In-house and invited experts gave lectures. The program of the To manage the structural changes and adapt to school was structured to provide the participants the changing system, it was decided to suspend all with a broad base knowledge of the Plateau de astronomical activity at the Observatory on August Bure Interferometer and its future upgrades and a 31, 2010. Operation restarted with 3 antennas (1, particular accent was given on ALMA. Participants 2 and 5) after two weeks of testing and bug fixing, had the opportunity to present posters on their own and was resumed entirely with all six elements work and discuss results obtained with the Plateau of the interferometer at the end of the antenna de Bure Interferometer to share their knowledge maintenance period (October 17, 2010). The only and learn from each other’s experience. The school drawback is the loss of a failing vertical polarization was limited to a total of 63 researchers from Europe mixer on antenna 1 because of an open-circuit. It is and overseas: Germany/ESO (19), France (13), planned to replace the inoperative mixer during the Netherlands (2), Spain (8), USA/Canada (4), Chile antenna maintenance period 2011. (4), United Kingdom (3), Denmark (2), Argentina (1), Finland (1), Italy (2), Bulgaria (1), Ireland (1), Portugal (1) and Switzerland (1). The lectures of the 7th DATA ARCHIVE Interferometry School and the proceedings from previous Interferometry Schools are available on the As in previous years, in a continuing and successful IRAM Web. The school received financial support effort with the Centre de Données astronomiques from the RadioNet (FP7) initiative of the European de Strasbourg (CDS), data headers of observations Commission. The funding was used to pay the meal carried out with the Plateau de Bure Interferometer costs for participants, accommodation and missions are conjointly archived at the CDS, and are available for the outside lecturers and accommodation for viewing via the CDS search tools. In 2010, the costs for selected participants. No school fees were archive contained coordinates, on-source integration charged to participants. time, frequencies, observing modes, array configurations, project identification codes, etc. for observations carried out in the period from January USER SUPPORT 1990 to May 2010. The archive is updated at the CDS every 6 months (May and October) and with a delay The Plateau de Bure Science Operations Group (SOG) Participants at the 7th Millimeter Interferometry of 12 months from the end of a scheduling semester is staffed with astronomers that regularly act as School astronomers on duty to optimise the scientific return Annual report 2010 25 RadioNet PI User Distribution 2 0 0 4 - 2 0 1 0 of the instrument, directly on the site or remotely RadioNet observing time was allocated to eligible from Grenoble, provide technical support and UK principal investigators from expertise on the Plateau de Bure interferometer to ITALY United Kingdom (percentage investigators and visiting astronomers for questions Netherlands of total time is 54%), Italy related to the calibration, pipeline-processing and Hunga ry (38%), the Netherlands (4%), Denmark (1%), Hungary (1%), archiving of Plateau de Bure data, interact with De nma rk Portugal (1%), Sweden (1%) the scientific software development group for P ortuga l and Switzerland (<1%) with a developments related to the long-term future of S w e de n slightly unbalanced distribution between PhD students and the interferometer, perform the technical reviewing Switzerland post-doctoral researchers (31%) of the proposals, and collaborate with technical and senior scientists (69%). groups to ensure that operational requirements are being met. Five astronomers were appointed to the to maintain an excellent reputation concerning group at the end of 2010. The group also received the assistance and service given by scientists and the support of Ivana Stoklasova-Orlitová, a visiting support staff to visiting astronomers. astronomer from Prague on a three months stay. VLBI NEWS In 2010 assistance was given to 30 investigators from Europe and overseas visiting IRAM Grenoble for a In early 2010, it was necessary to re-test the Plateau total of 130 days to reduce data from the Plateau de de Bure VLBI capabilities: the arrival of WideX had led Bure Interferometer. Advice and support was also to numerous hardware and software modifications provided to a number of experienced astronomers that could have impacted the VLBI part. Instead of from Bonn, Bordeaux, Cambridge, Garching, fully disabling WideX in VLBI mode, it was decided Heidelberg and Caltech to reduce and analyze to keep it as a parallel backend for pointing, focus Plateau de Bure Interferometer data remotely and flux estimates. It turned out to be impossible to from their home institutes. Having suffered from a fully align both WideX polarizations in phase while severe computer network attack early this year, the in VLBI mode: the phase offsets would impact the protection of the IRAM’s computer network was narrowband correlator during a phasing observation, reviewed and it was decided to limit remote access and lead to a wrong alignment of the individual to specific machines for data reduction purposes. antenna phases during VLBI. Real-time pointing and focus had therefore to be limited to one WideX polarization only, but even so, the tremendous gain RADIONET USERS in bandwidth (3.6 GHz compared to the 128 MHz of the narrowband correlator in VLBI mode) provided Since January 2004, travel funds have been made a significant improvement. For the offline flux available to RadioNet eligible astronomers from non calibration, it was possible to calibrate the phases IRAM partner countries for expenses incurred during separately and thus use both polarizations. their stay at IRAM for reducing data from the Plateau de Bure Interferometer. These funds which were During the Global Millimeter VLBI Array (GMVA) initially made available by the European Commission campaign on May 6-11, both IRAM observatories in the frame of the FP6 program, are today managed suffered from difficult weather conditions. Pico by the FP7 program. For the year 2010, the Program Veleta observed 53% of the scheduled scans, and Committee received 27 eligible proposals and Bure 50%. When not counting the scans impossible recommended 15 proposals for observations with for Bure due to the sun avoidance of 35 degrees, the Plateau de Bure Interferometer. Taking into the Bure fraction improves to 54%. This relatively account proposals accepted in 2008 and 2009 but small difference shows that the reduction of the sun continued in 2010, time was allocated to 14 eligible avoidance circle from 45 to 35 degrees for the winter proposals corresponding to a total of 266 hours of 2009/2010 season had a positive impact on the observing time. Since the beginning of RadioNet, rather rigid VLBI observing schedule. access time was allocated to 78 eligible proposals (12 in 2004, 11 in 2005, 11 in 2006, 13 in 2007, 14 In the October 8-11, 2010 GMVA session, the in 2008 and 6 in 2009) for observations with the respective observing fractions of Pico Veleta and Plateau de Bure Interferometer, corresponding to Bure were of 33% and 94%. Previous tests in 2010 a total of ~1900 hours (272 in 2004, 239 in 2005, had shown that both IRAM observatories were 272 in 2006, 326 hours in 2007, 334 in 2008 and capable of doing VLBI at 230 GHz. After the end of 140 in 2009) of observing time. User responses to the Global campaign, the PI of a pending 230 GHz questionnaires of the EU show that IRAM continues VLBI project asked explicitly to start the project 26 Institut de Radioastronomie Milimétrique although the conditions were sub-optimum (the Around the time of the installation of the principal source was about to enter a long sun astronomical Band 4 receivers, an occasional avoidance period). Even so, fringes of high quality interference problem was noticed on the low- were found, which proves that (i) the Bure array frequency channel of the radiometers. Triangulation phasing works at a sufficient stability and (ii) that the experiments showed that the source was likely to Bure LO chain with its R&S SMA100 B22 frequency be inside the receiver cabins, and was traced to synthesizer at the place of the Racal Dana can a component of the new Band 4 LO boxes that successfully operate at high frequencies. enters the first radiometer band above a certain Band 4 observing frequency. Three simultaneous In late 2010 it became necessary to refill the approaches were put in place to reduce the impact: hydrogen storage of the Plateau de Bure EFOS-38 (i) setting the frequency of the LO box on a safe maser: the hydrogen storage monitoring showed a «parking position» when Band 4 is not used, (ii) telltale non-linear drop that indicated a remaining developing a passive shielding in the LO box; a first operation time of a few months. The refill operation antenna is already equipped and shows that the was done on the mountain by a T4Science approach is efficient, and (iii) the development of technician. The maser was back into operation after an offline “dual frequency” radiometer scheme that a few hours and is working fine since then. allows to recover most of the continuum phase correction on contaminated data. Considering that Band 4 observations are typically scheduled when THE 22GHz RADIOMETRIC the atmosphere is already close to perfection, the PHASE-CORRECTION SYSTEM impact of the interference has been very limited. The 22 GHz radiometer system on the Plateau de On the subject of the phase correction tools, Bure antennas underwent several improvements substantial progress has been made in the extension in 2010. In June, the radiometer on antenna 3, of the time range of the phase correction. These which showed a dysfunction in its load arm and an tools are so far experimental, but will soon enter the elevation-dependent gain drift, was replaced by the main CLIC distribution. spare. The problems were resolved in the Grenoble frontend laboratory, so that a fully functional spare is again available. New control cards based on the NTP antenna time solved the PPS timing problems that had been noted in particular on Antenna 2. In the real time acquisition, a command was introduced to enable or disable a sliding three-second averaging window on the raw radiometer data. This allows trading time resolution against a better signal-to- noise of the phase correction when the atmosphere is very stable, and was successfully applied from December 2010 on. Annual report 2010 27 Grenoble headquarters SIS GROUP The development of thin films and structures for kinetic inductance detectors (KIDs) has grown into During 2010, the fabrication of the total number of a major activity during 2010. Various designs of required SIS junctions for the ALMA Band 7 project lumped element KIDs were produced and different has been successfully achieved and the focus of qualities of aluminum film parameters explored. the group has shifted to new developments and The produced detectors allowed a second run with projects. New designs of junctions for broadband the NIKA instrument in October 2010 with greatly 2SB mixers in the 230 GHz window, as foreseen improved sensitivities at 2mm. Other very promising for NOEMA, were fabricated and work to stabilize materials such as NbN and TiN have been explored the process yield for multi-junction devices and essential process steps such as film deposition continued. In early 2010, the SIS group accepted and and etching as well as film characterization utilities commissioned a new deposition system (PLASSYS has been established. Work on passive millimeter 500S) that will allow considerable improvement of wave structures using silicon technology and surface thin film development by exploring new material mounted MEMS technique was pursued. Deposition and process combinations unavailable so far. The of Si and SiN membranes and their patterning deposition system has been custom designed started with the goal to support advanced millimeter and enables easy change of sputter targets while wave-guide coupling structures as designed by the combining RF/DC sputtering with a multi crucible IRAM receiver group. Ongoing work to improve Ebeam evaporation station. The machine provides the process for metallic surface mounted variable fully programmable automatic process control capacitors addressed the ‘sacrificial layer’ preparation and was one of IRAM major investments in 2010. and release process. Change of superconducting transition temperatur Tc depending on N2 flow during plasma sputter deposition for the two binary nitrides TiN and NbN. These materials are of particular interest for kinetic inductance detectors. Right: Combined Sputter/ Ebeam-Evaporation system commissioned during early 2010. New materials and film combinations will be one of the main goals with this equipment. 28 Institut de Radioastronomie Milimétrique FRONTEND GROUP The characterization of the Band 4 RF modules (275-373 GHz band) was completed in the lab and The year 2010 was a busy year for the Front receiver noise measurements were performed End group with maintenance, upgrade, and using one of the new electronically tuned Local development activities for both IRAM observatories. Oscillators (see below). The Band 4 RF modules were Local Oscillators (LO) and cryogenic RF modules installed in antennas 1, 2, 3 and 6 (not yet equipped for Band 4 were installed on the Plateau de Bure in 2009). The Band 4 RF module of antenna 4 (with antennas and the LO modules of Bands 1, 2 and a SIS junction in open circuit after a cool down) was 3 were modified to be compatible with the new replaced with a new one. In antenna 1, one of the reference (LO1ref). A 3 mm HEMT receiver was built two SIS junctions of the 2SB mixer Band 4 module of and installed on the Pico Veleta telescope and a new V polarization is open-circuited. mixer for EMIR Band 3 was developed. Construction of a spectrum slicer for a FFT backend has started A new first LO reference signal (13.2-16.4GHz - and good progress was made on the design of the 3 LO1ref) for the mm-waves local oscillator modules mm band 5x5 multibeam receiver, both for the Pico was developed by the IRAM backend group and Veleta telescope. all mm-wave LO modules of Bands 1, 2 and 3 were modified to be compatible with the new reference. New harmonic mixers with integrated diplexer were PLATEAU DE BURE INTERFEROMETER developed and installed inside existing LO modules UPGRADE AND MAINTENANCE to replace old units. The modified LO modules (3 Two cryogenic cold heads were replaced on Bands x 6 antennas plus spares) were installed on antennas 5 and 6 after four years of continuous the Plateau de Bure antennas in September 2010. operation. Following degradation in performance, one of the 22 GHz water vapour radiometers was replaced with a spare unit. A 4-8 GHz cryogenic ELECTRONICALLY TUNED LOCAL amplifier was replaced in antenna 1 after installation OSCILLATORS FOR PLATEAU DE BURE of the new Band 4 RF module. BAND 4 A series of eight 283-365GHz electronically tuned Local Oscillators (LO) for Band 4 of the Plateau de Band 1 Local Oscillator module modified with new Bure interferometer was built and characterized. harmonic mixer (highlighted by red rectangle). The design of the Local Oscillator, described in previous annual reports, is based on a commercial 15.7-20.3GHz YIG oscillator cascaded with an active multiplier chain (AMC) and a 3 mm band power amplifier (PA) module built at IRAM. AMC and PA both integrate 94.3-121.6 GHz MMIC amplifiers Below: Details of a 67-118GHz harmonic mixer showing the EBPA107C from NRAO. A commercial frequency chip and its integration in the mechanical block with tripler, with efficiency of the order of 3%, delivers the diplexer frequency circuit. final frequency signal. The tripler is cascaded with a cut-off attenuator which reduces the LO noise contribution to a level comparable to that delivered by a Gunn oscillator. The measured output power of the 3 mm band LO module (before tripler) is in the range of 8-50 mW. The output power across 283-365GHz, after a ~4 dB room temperature attenuation, lies between 50 and 270 μW for all eight LO modules of the series; this output power is large enough to pump the Band 4 Sideband Separating SIS heterodyne receivers. The new Band 4 LO system, compatible with the new 13.2-16.4GHz first LO reference, allows to phase- lock on a time scale of order of few seconds (to be compared with the few minutes required with the mechanically tuned Gunn oscillators). The new Local Oscillators were successfully installed on the Plateau de Bure interferometer antennas and Annual report 2010 29 the first astronomical observations were performed At room temperature, the signal is then filtered, across Band 4 in late 2010. The new system opened down-converted and further amplified to provide up the sub-millimeter wave window at Plateau de a final 8GHz IF bandwidth across 4-12GHz, which is Bure. This was the first time that a YIG-based Local compatible with the currently available IF processor. Oscillator was used at the IRAM observatories. The noise temperature (SSB) of the HEMT receiver measured in front of the cryostat window is about A 3 MM BAND HEMT RECEIVER 55 K across the whole 84-116 GHz frequency range PROTOTYPE FOR THE 30-METER (see figure). The measured total power stability (Allan TELESCOPE deviation) is below 3.10-4 for integration times in the The 3 mm band Local Oscillator module. A 3 mm band (84-116 GHz) HEMT receiver prototype, range 1-100 sec, better than the specification of the designed and constructed at IRAM, was installed ALMA receivers. at the 30-meter telescope in August 2010. This receiver allows us to test the 3 mm band cryogenic InP MMIC amplifiers technology and to compare its performance with that delivered by the Sideband Separating SIS mixers (2SB) already available at the site (E0 band of the EMIR receiver). Inside the telescope cabin, a movable flat mirror switches the telescope beam from the HERA receiver to the 3mm HEMT receiver where it is redirected inside the cryostat and coupled into a single corrugated feedhorn whose output is cascaded with an orthogonal mode transducer from NRAO. Two MMIC HEMT amplifiers from University of Massachusetts, cryogenically cooled to 15K, amplify the 3mm signal in each polarization channel. Above: Series of seven 3 mm band LO modules and their power supplies. Left: Spectrum of the Local Oscillator signal at 298.2 GHz. Right: Output power of the eight 3 mm band LO modules. 30 Institut de Radioastronomie Milimétrique EMIR BAND 3 MIXER UPGRADE A new sideband-separating (2SB) 200-280 GHz SIS mixer with a 4–12 GHz IF band was developed within the European FP7 RadioNet AMSTAR+ work package. The goal of this work package is the development of receiver pixels and LOs for large focal plane arrays. Therefore, the mixer was designed in a very compact way and the usually adopted superconducting coils for the suppression of the Josephson effect were replaced by permanent magnets. The RF part of the 2SB mixer consists of an RF coupler/mixer block combining all waveguide couplers and the two double sideband SIS mixers in one E-plane splitblock. A 4-12GHz IF hybrid coupler developed by CAY also within AMSTAR+ can be connected directly to the 2SB mixer module. The mixer has been designed to work for RF frequencies between 200 and 280 GHz and over an IF band of 4–12 GHz. Tests of a prototype have shown that the mixer performs very well (see The 3 mm band HEMT figures) over the design frequency range and even receiver installed in the beyond with a flat response across the IF band. The receiver cabin of the 30-meter telescope. average image rejection lies around -14 dB. This new mixer will replace the currently installed SSB mixer with 4 GHz IF band of EMIR Band 3, thus quadrupling Receiver noise temperature the instantaneous bandwidth of the receiver. (left scale) and gain (right scale) integrated over the 4-12 GHz IF band. The blue curve refers to horizontal polarization, the red one to SPECTRUM SLICER FOR THE 30-METER the vertical polarization. TELESCOPE FFT BACKEND An IF processor allowing to interface the IF bands from either the EMIR or the HERA multibeam Photograph of one half of the The receiver was successfully used to perform receivers to a Fast Fourier Transform (FFT) sideband separating mixer preliminary astronomical observations. spectrometer from Radiometer Physics GmBH unit showing the RF coupler/ mixer block (left) and a close- is being developed. Two modes are possible: up of the mixer chip and permanent magnets (right). “wideband mode” (4 GHz bandwidth, 200 KHz resolution), and “high resolution mode” (50 KHz resolution, 1.8 GHz bandwidth). The instrument will be able to process eight inputs simultaneously, i.e. 8 x 4GHz=32GHz maximum in wideband mode. During 2010, the design of the spectrum slicer was completed and a set (24 plus spares) of locked local oscillators was built and tested; then, the first prototype of a complete subunit was put together. Annual report 2010 31 FOCAL PLANE ARRAY RECEIVER FOR THE 3 MM BAND ON the 30-METER TELESCOPE A 5x5 multibeam receiver for the 3 mm band is being designed for the 30-meter telescope. The receiver will be based on a modular design with broadband input optics, dual linear polarization ortho-mode transducers and sideband separating (2SB) SIS mixers. The design includes a field derotator, which will allow to track the parallactic angle. The study of the overall cryostat design and receiver implementation into the telescope cabin is in First prototype of a complete spectrum slicer sub-unit, consisting of a local oscillator (left), two progress, as well as the design of the local oscillator isolators (small black cases), a cavity bandpass filter (big black case), a mixer (smallest case, in the center), baseband electronics (big cases, top), around two anti-aliasing lowpass filters (the two distribution scheme into the RF module. Several rectangular items with golden body) and, on the right, the output amplifier. A total of 24 sub-units optical prototype components were fabricated by are to be built to complete the project. the IRAM mechanical workshop (corrugated feed horns and double-face mirrors of individual optics). ALMA BAND 7 CARTRIDGE PRODUCTION IRAM is responsible for the production (component fabrication and procurement, assembly and test) of 65+8 spares ALMA Band 7 cartridges covering the RF signal frequency range 275-373 GHz. The dual polarization receivers employ Sideband Separating (2SB) SIS mixers and deliver 4GHz IF band per sideband. The middle of the cartridge production was reached towards the end of 2010. During 2010, nineteen receivers with state-of-the-art performance were delivered and accepted by the project. Left: Preliminary design of the 5x5 pixels cryogenic RF module. Above: Design of broadband turnstile junction waveguide ortho-mode transducer. Below: Prototype five-pixel optics (feed-horns and double-face mirrors). 32 Institut de Radioastronomie Milimétrique Backend Group electrical power distribution was required. Soon after its connection, the new correlator was made In 2010, the backend group successfully delivered available for commissioning and then offered to the the new correlator (Widex) to the Plateau de Bure community for the observations. interferometer and continued its work to prepare for the next generation of correlator. During eleven months of permanent operation, only one minor failure was reported. None of the correlator chips showed any sign of dysfunction. WideX Correlator delivered on Widex is built to accommodate 8 antennas and Plateau de Bure is currently operated at 15/28 of its capacity. A On February 10 2010, all four quarters of the new complete description of Widex can be found at correlator WideX were installed on the Plateau de Bure correlator room and successfully connected http://www. iram.fr/IRAMFR/TA/backend/WideX/ to the rest of the system. An improvement of the index.html New LO transport system The phase-stabilized reference frequency for tuning the receivers 1st LO’s was moved from the 2 GHz Above: One of the ALMA Band range to 16 GHz. This new frequency plan allows 7production cartridges. a fast and easy tuning and, in addition, suppresses some spurious lines that were internally generated. It Right: Performances of the 19 ALMA Band 7 cartridges uses a YIG oscillator that provides a more consistent delivered in 2010. performance than the previous mechanically (Above) Noise temperature integrated over 4-8 GHz IF tuned DRO’s. All six antennas of the Plateau de Bure versus LO frequency. The ALMA specification of 147 K interferometer have been equipped with this new SSB noise, indicated by the horizontal red line, is well LO transport system and the production run has above the measured values. made provision for 6 others. (Below) Image sideband rejection versus signal frequency measured at five different LO frequencies. Polarimetry Six PIN transfer switches and their driving circuitry were installed on the Plateau de Bure interferometer. Every second, they allow one to swap the H and V IF’s, according to a Walsh function sequence, so that the source polarization information can be extracted. View of Widex in the correlator room of the Plateau de Bure interferometer DiFER project Technology for the next (5th) generation for an IRAM correlator is currently under study. A board has been designed that includes a 5-bit, 8 Gsample/sec ADC and a powerful FPGA. It will be used to acquire expertise on synchronization of multiple, multi gigabit data streams. Concomitantly, a polyphase filterbank was designed and simulated. This polyphase filterbank is able to digitally split a 4 GHz band into 64 frequency windows. These elements are the building blocks for a future correlator, featuring high versatility in trading bandwidth versus resolution, and integrating phased array for wideband VLBI. Further information on this new project can be found at http://www. iram.fr/IRAMFR/TA/backend/WideX/ index.html Annual report 2010 33 MECHANICAL GROUP ■■ Leading, with the team in Granada (Spain), the refurbishment of 1 Azimuth and 1 Elevation In 2010, the staff of the mechanical group dealt with gearboxes at the 30-meter telescope. 148 requests for mechanical components. Many of these requests were handled internally, and only a Technical support for antennas fraction was subcontracted to outside companies. As in previous years, the technical group closely A view of the HEMT Receiver in the Frontend laboratory collaborated with the technical staff on the Plateau before shipping to the de Bure for all aspects dealing with the antennas. 30-meter telescope Workshop The workshop produced a large number of microwave components, mixers, couplers, and horns for the new generation receivers of the Plateau de Bure interferometer, AMSTAR couplers, and HEMT components. The workshop carried on with the production of the components in the frame of the ALMA Band 7 construction. Despite the tight schedule, the fabrication of the elements was done on time as foreseen. The workshop was equipped with a new quality control device that optimises the quality control procedure. Design Office New Cad files data organisation The design office succeeded to install a Product Lifecycle Management process dedicated to the 3D Cad files – Solidworks PDM workgroup. Included with the current CAD software, it will play a key role in managing projects, control design revisions and control data access. This software resulted in improving significantly the quality process. NOEMA project Progress was achieved on various mechanical projects to upgrade the Plateau de Bure antennas in view of the NOEMA project. In 2010, the main projects dealt with the following issues: ■■ Weight reduction on reflector ■■ Production cost reduction ■■ Back Up Structure of Subreflector ■■ Roller cable Microwave and antenna studies In close collaboration with other groups at the institute, the design office worked on numerous mechanical designs that concerned: ■■ Design of new microwave components for Plateau de Bure and the 30-meter telescope ■■ Design and installation of HEMT receiver ■■ Leading the manufacturing of 2 set of panels for 2 new reflectors for the Plateau de Bure antennas 34 Institut de Radioastronomie Milimétrique IRAM ARC NODE program. In that context, a new wide-field imaging technique was developed during the last years to .The IRAM astronomy support group is involved be able to properly process large maps obtained in several ALMA-related activities and software with On-The-Fly interferometry. This technique is developments, which are part of a more general being implemented and tested in GILDAS. In 2010, effort to develop a node of the European ALMA the work for the implementation in the ALMA data Regional Center (ARC). reduction software, CASA, was started. IRAM is deeply involved in the development of one IRAM and ESO agreed on a scheme allowing of the key software for the real-time operations of IRAM astronomers to participate to the ALMA ALMA, the Telescope Calibration (TelCal) software. commissioning and science verification phase. This software is performing all real-time calibrations Following that agreement, an IRAM astronomer necessary to run the array: antenna pointing, spent three months in Chile in summer 2010. This focus, baseline measurements, atmospheric was a very fruitful experience, and as a consequence, parameters, etc. Two IRAM engineers are working the visit of two other IRAM staff members to the on this development. 2010 was a critical year for Joint ALMA Observatory in Chile is planned in 2011. TelCal, as the array commissioning made large progresses, implying a continuous and important The planning and preparation of the IRAM ARC effort to correct, adapt, and maintain TelCal. New node has continued. While the European ARC functionalities were also added, as atmospheric core activities are based at ESO Garching, IRAM is calibration using loads at several temperatures. one of the European scientific support nodes. The Finally, a stand-alone version of TelCal, interfaced to tasks of an ARC node is mostly to form the users to the CASA off-line package, is also being developed, the millimeter interferometry techniques and to to allow an off-line reprocessing of the real-time the ALMA instrument, and to provide face-to-face calibration. support for the data reduction after the data have been acquired. In that context, IRAM intends to build During 2010, IRAM was also involved in the on the existing in-house expertise on millimeter development of the Observatory Operations interferometry techniques and on the experience Support (ObOps) package. This is a suite of software acquired with the institute participation to the tools developed to support the handling of the ALMA construction. The face-to-face support service observing programs, from the Call for Proposals to provided to Plateau de Bure interferometer users for the project completion, as well as the day-to-day more than 15 years will be extended to ALMA. real-time operations. Participants of the “Observing with ALMA: Early Science” A major achievement during 2010 was the workshop held in Grenoble The institute is also responsible for one work organization of the “Observing with ALMA: Early on November 29 – December 01, 2010. package of the EU-funded “ALMA Enhancement” Science” workshop, that took place in Grenoble, November 29 to December 1. During three days, many practical aspects of the ALMA instruments were discussed and explained to the participants, as, e.g., the time allocation committee, the pipeline, or the key software astronomers will have to use. More than 180 persons registered to that meeting, a large number that required organizing this event not at IRAM but in a larger, more convenient location in Grenoble. On the long term, having access to the Plateau de Bure/NOEMA and to the ARC node services should place the IRAM users community in the best possible position to get time on ALMA in an extremely competitive environment. Annual report 2010 35 COMPUTER GROUP upgrade of the receiver software. A new simulator window was included and new control and status In the frame of the installation of the new prototype commands were added. This installation provided an receiver called HEMT at the 30-meter telescope, opportunity to improve the software performance the computer group was involved in the support by getting rid of Python and by writing everything in of the control and monitoring software. The main C++/Qt. Still, in order, to standardize our distribution features include two specific graphical interfaces for at the 30-meter telescope and the Plateau de Bure the laboratory and the observations, an automatic interferometer, the same protocols, SQL database LO tuning, a build-in simulator, an embedded SQL and XML/RPC, are in use. database for configuration storing, a XML RPC server for easy integration with the existing observing In general, all front-end software was updated in software. The package was written in C++/Qt. 2010 and improved to comply with this software framework. At the Plateau de Bure interferometer, the 22GHz water vapor receiver software was modified to rely In Grenoble, a study showed the difficulty to on the IRAM Network Time Protocol (NTP) timeserver continue to work with a Fedora distribution for Linux, for triggering the integration periods and flagging as the versions were changing too rapidly and the the measures. The old wired time bus was found security support was too short. A free distribution, unreliable for far distant antenna stations. Scientific Linux, was therefore tested. The releases are synchronized with RedHat Entreprise and their The Polar switch module with is software was also lifecycle is up to 10 years. The selected release 5.5 of installed on the Plateau de Bure interferometer. May 2010 is now the version installed on the new A GUI and XML/RPC commands let the users and machines and was available on the 15 personal applications select the polarizations connected to computers that were set up for the interferometry the correlator. summer school. The installation of the Band 4 receiver at the Plateau A new NAS with a raw volume of 5TBytes was added de Bure interferometer with its specific LO, based for the astronomer user space and the projects. on a YIG tuned oscillator, required a substantial 36 Institut de Radioastronomie Milimétrique As a consequence more space is available to the important changes in the acquisition and data technical and administration staff. reduction steps. For instance, MIRA was upgraded to 1) work in 64 bits mode to benefit from modern Our IT disaster recovery plan has shown the need computer technology and 2) process smaller chunks of backing up most of our NAS data space. While of data (subscans instead of scans) to obtain a better the data from the Plateau de Bure interferometer synchronization between data acquisition and data is well protected with redundant disks and multi processing. This latter improvement is useful to servers located at different places, the NAS user data check long scans (e.g., pointing, OTF) at intermediate spaces had no backup. Although the NAS is reliable steps. The advent of broadband spectra at high in its concept nothing could be saved on magnetic spectral resolution considerably eases multi-line media. The volume to backup is in the order of studies. This triggered a series of changes in the 4Tbytes! A solution with RAID 0 servers was set up. data processing and analysis of such spectra in They are linked with optic fiber to the NAS and CLASS. For instance, the possibility to select all the located in the building basement as far as possible spectra of a file whose frequency axis intersects a from the computer room. The backup performed given frequency range was introduced. Interfacing over the weekend sustains a transfer rate better than line databases (JPL, CDMS, ...) to identify the lines 300Gbytes/s. and to model their properties converged. It was developed in collaboration with the Observatoire de An effort is still done to distribute automatically Grenoble and it was released as a CLASS extension, Windows applications or patches. In connection named WEEDS. The EMIR broadband receivers have with this distribution, the new accounting software a rejection level of only 13dB. In addition, broadband release has been worked out to ease its installation. receivers in the sub-millimeter (e.g., some Herschel/ HIFI receivers) are double-side band. This implied Finally, in order to unify the authentications and the resurrection of double-side band possibilities the information needed to the different OS’es of CLASS. The software package MOPSIC, which is and applications, a development was started that used to 1) monitor the 30-meter telescope behavior is based on LDAP (Lightweight Directory access and 2) support the bolometer observations, was Protocol) servers with common records among maintained. Finally, the new generation of 30-meter the Windows and Unix implementations. For telescope time/sensitivity estimators introduced authentications, a master Kerberos server is the last year for EMIR was extended to the HERA and solution that has been retained. MAMBO cameras. At the Plateau de Bure interferometer, three main SCIENCE SOFTWARE ACTIVITIES hardware changes happened in 2010. First, the new broadband WIDEX correlator was installed. Second, The first goal of the science software activities at the 0.8 mm receivers (Band 4) were commissioned. IRAM is to support the preparation, the acquisition This implied a change of the local oscillator system. and the reduction of data both at the 30-meter and As a consequence annoying parasites were the Plateau de Bure Interferometer. This includes suppressed and the phase stability increased. Last, the delivery of 1) software to the community for polarimetry measurements were made possible proposing and setting-up observations, 2) software through the installation of a device, which switches to the IRAM staff for use in the online acquisition the antenna inputs of the correlators. This enables system and 3) offline software to end users for final the system to measure the different polarimetry reduction of their data. However, the GILDAS suite products in a given time sequence. All these of software is freely available to and used by other hardware changes implied software changes in the radio telescopes. setup, acquisition and reduction of the observations. Specifically, ASTRO was upgraded to reflect changes At the 30-meter telescope, the main event of 2010 of the frequency plan induced by the change of was the introduction of the first two units of a the local oscillator system. The softwares to pilot new backend technology called Fourier Transform the WIDEX correlator, the frequency synthesizer Spectrometer (FTS). In combination with the EMIR and the polarimetry switch box were finalized. The receivers, these units allow the observer to obtain other online acquisition softwares (in particular OBS, spectra at a spectral resolution of about 200 kHz RDI and CLIC) were also adapted. A large effort was on a bandwidth of about 4 GHz. This amounts to needed to upgrade the pipeline, so that it continues about 20000 channels per unit. In the next two years, to optimally calibrate most of the projects. the 30-meter will be equipped with up to 16 such units. This will represent an increase of the data rate Collaboration with the Observatoire de Bordeaux by almost one order of magnitude, which implies was started to implement inside CLIC the calibration Annual report 2010 37 of interferometric polarimetry. In the area of imaging conferences at St. Etienne-en-Dévoluy (in the Hautes- and deconvolution, IRAM leads the research and Alpes near the Plateau de Bure). development activities around the interferometric On-The-Fly observing mode in the framework of After the brochure and the web page, the IRAM the European FP6 program ‘’ALMA Enhancement’’. Newsletter got an overall “re-looking”. It is published In 2010, the first steps of a new algorithm to image twice a year (in February and July). The new edition, interferometric On-The-Fly data were implemented. called “IRAMInfo”, has a completely new layout and is In parallel, the acquisition of On-The-Fly data at the only available electronically. Special emphasis is given Plateau de Bure interferometer was improved and to scientific results, technical developments and new tests were made. Finally, the configurations of reports on the large observing programs. the ALMA GILDAS simulator were upgraded to reflect the advancement of the project construction. At the end of spring, preparations for the 7th IRAM Interferometry Summer School started. The school All these developments are based on the common took place on October 2010 with more than 70 GILDAS services, e.g., a set of common low-level participants and lecturers working together during libraries, collectively named GILDAS kernel, which open sessions and tutorials. takes care of the scripting and plotting capabilities of GILDAS. Although any effort in this area is Right after the Summer School, the IRAM ARC Node not necessarily visible for the outside world, it is organized a workshop about Early Science with extremely important for the life of the IRAM data ALMA. During three days, more than 140 participants reduction software. In 2010, the large effort to and lecturers exchanged information and latest news overhaul the graphical possibilities of GILDAS was about ALMA, the first call for proposals and early continued so that it could be released in 2011. This observations. is a step required to cope with the large increase of data size, which will result from both the improved At the end of the year, IRAM took part, for the second imaging capabilities of the IRAM instruments and the time, in the French national science festival Fête de increase in the number of channels of the upcoming la Science. With an interactive and movable model generation of spectrometers. Finally, the support of of the Plateau de Bure Interferometer, a 3-D film, live the more and more popular GFORTRAN compilers observations with a telescope in Sweden (thanks to and Mac/OSX system was improved. the Hands-On-Association) and presentations about our Solar System, the institute’s exhibition stand This impressive number of concomitant software attracted a lot of visitors. About five school classes developments is a testimony to the vitality of the per day and more than 11000 people in total visited team of software developers, which was largely the IRAM stand. renewed during the last 5 years. PUBLIC RELATIONS The year 2010 began with two very spectacular press releases, which both triggered a major echo in the international press. For the first time, it had been possible to pinpoint the location of water in a very young proto-planetary system, analogue to our Sun – thanks to the IRAM Plateau de Bure Interferometer. In addition to this result, another paper was published in Nature reporting the detection and imaging of cold molecular gas in star forming galaxies representative of galaxy populations shortly after the Big Bang. International media picked up both results and IRAM had several articles in international newspapers like the German FAZ, the FOKUS and Scientific American. In order to continue public outreach work on a regional level, IRAM astronomers continued during all winter season their well-attended series of public 38 Institut de Radioastronomie Milimétrique Personnel and finances Japanese women playing with a telescope. Early 19th century Japan. The IRAM administration comprises 3 groups in FINANCES charge of the areas as of human resources, finances and general services. The activity of the IRAM administration in the area of finances covers the budget preparation and management, the annual accounts and the liaison HUMAN RESOURCES with the auditors and the audit commission. The overall is reported on a yearly basis to the Executive In 2010, 105.5 positions were foreseen in the Council. personnel plan authorised by the IRAM Executive Council, i.e. 77.7 for France and 27.8 for Spain. 11 IRAM’s financial situation in 2010, as well as budget additional positions are authorised for Post-docs and provisions for 2011, are summarised in the following thesis students. tables. In addition to these authorised positions, IRAM also The associates approved a 2% increase in their base has a number of staff recruited for specific activities contribution to the operational budget of 2010. They such as ALMA contracts and European contracts. also agreed upon a further increase by 2% for 2011. The contributions to the investment budget were In total, IRAM employed a total of 146 persons (132 maintained at their previous level for 2010 and 2011. FTE) in 2010. In addition, the associates finance the reconstruction of the cable car to access the plateau de Bure observatory. The IRAM administration completed a global review of the IRAM insurance package that was started in 2009. The revision is now finished and a new company has been hired to deal with IRAM insurance. Annual report 2010 39 Income and Expenditure Income 2010 - 2011 (in keuros) Budget heading 2010 2011 CNRS contributions 9 148 7 178 MPG contributions 6 148 5 678 IGN contributions 785 725 TOTAL 16082 13582 Carry forward from previous years 3 080 5 161 IRAM’s own income 1 252 1 438 Other incomes (Equipex) 1 000 TOTAL INCOME 20 414 21 181 Expenditure 2010 - 2011 (in keuros) Budget heading 2010 2011 Operation / Personnel 7 869 8 086 Operation / other 3 873 3 791 Investment (base + special) 3 491 9 305 TOTAL 15 233 21 181 Budgetary Excess 5 182 TOTAL EXPENDITURE 20 414 21 181 40 Institut de Milimétrique Annex I TELESCOPE SCHEDULES The next two tables show the allocations for the telescope time for the 30-meter telescope and the Plateau de Bure interferometer for the year 2010. In each table, the first column gives the project’s identification, the second column the title of the investigation and the third column the names of the Principal Investigators and the co-Investigators. 30 metre telescope Ident. Title of Investigation Authors 212-08 HERA Maps of KINGFISH Herschel Key Program Walter, Leroy, Schinnerer, Rix, Weiss, Kennicutt, Calzetti, Schuster, Wiesemeyer, Schruba Galaxies 057-09 Origins of molecular clouds and star formation in Motte, Schilke, Nguyen, Schneider, Bontemps, Schuller, Menten, Wyrowski, Heitsch, Hennebelle, Banerjee, W43 - a large HERA project Kramer, Simon, Beuther, Henning, Bronfman, Walmsley, Zavagno 149-09 Vertical distribution of CO in the deep atmosphere Moreno, Lellouch, Marten, Paubert of Neptune 150-09 CO in Enceladus and in the E-ring of Saturn Cavalié, Greaves 151-09 Cometary observations in support to the Herschel Biver, Crovisier, Bockelée-Morvan, Colom, Moreno, Hartogh, Lis, Boissier, Paubert mission 154-09 HDO in the intermediate-mass protostar OMC2- Kama, Maret, Crimier, Ceccarelli, Dominik FIR4 155-09 Completing a detailed dust and che-mical study of Frau, Girart, Beltrán, Morata, Masqué, Alves, Busquet, Sánchez-Monge, Estalella, Franco the Pipe Nebula Cores 158-09 Confirming the core mass distribution constructed Peretto, Fuller, André from IRDC extinction maps 159-09 Tracing Dense Gas in IRDCs: A Prelude to Herschel, Linz, Vasyunina, Schmiedeke, Pavlyuchenkov, Krause, Beuther, Henning Act II 160-09 The role of environment on the formation of Orion Maret, Megeath, Stanke, Osorio, Tobin, di Francesco, Fischer, Poteet protostars 161-09 Understanding the Origin of a Remarkable Hacar, Tafalla, Quintana-Lacaci, Kauffmann, Kovacs Condensation 162-09 Dense Core Formation in the Brightest Taurus Hacar, Tafalla, Quintana-Lacaci, Kauffmann, Kovacs Filament 165-09 Assembling molecular clouds: mm continuum and Beuther, Kainulainen NIR extinction 167-09 CN Zeeman Measurements Towards High Mass Pillai, Menten Dense Cores: A Pilot Study 168-09 Magnetic field diagnostics in MSX IR dark clouds: 1. Poidevin, Wiesemeyer, Bastien, Vastel A search for Zeeman tracers in CL04 169-09 Measuring the magnetic support in the NGC 2264- Maury, André, Thum, Wiesemeyer, Peretto, Hennebelle C protocluster 170-09 Magnetic fields in massive star-forming regions: Beuther, Linz, Henning, Crutcher Testing the C2H Zeeman effect 171-09 C2H: a new opportunity to measure magnetic field Padovani, Walmsley, Tafalla, Galli, Thum in dense cores 172-09 Polarization study of CN emission towards massive Herpin, Bontemps, Wiesemeyer, Motte, Jacq, Schneider, Csengeri protostars: what is the role of the magnetic field? 174-09 Disk-Halo interaction: The foot point of the ‘’Giant Riquelme, Amo Baladrón, Martín-Pintado, Mauersberger, Bronfman, Martín, Burton, Jones, Cunningham Molecular Loops’’ at the Galactic center 178-09 A Comparison of Gas and Solid Phase CO Fraser, Craigon, Noble, Miller, Thi Distribution in Molecular Cores 180-09 The chemical structure of Orion : Completion of the Marcelino, Cernicharo, Bañó, Palau, Tercero, Guélin 2-D line survey at 1mm 181-09 Chemical complexity in strongly UV-illuminated Goicoechea, Fuente, Cernicharo, Bañó, García-Burillo, Usero, Berné, Marcelino regions 182-09 An Unbiased Spectral Survey of the Cep E Lefloch, Pacheco, Ceccarelli, Cernicharo, Hilyblant, Codella, Cabrit, Schuster, Loinard, Gueth, Fuente Protostellar Outflow - 184-09 The quest for CN and C2H - in space Agúndez, Cernicharo, Guélin, Mccarthy, Thaddeus 188-09 Search of CH₂D+ : deuteration in warm conditions. Roueff, Gerin, Lis, Wootten, Guélin, Cernicharo, Marcelino 189-09 Investigating the incredibly large deuteration ratio Parise, Sakai, Yamamoto, Müller in formaldehyde in L1527 190-09 Multiple deuteration of CH3CN in IRAS16293-2422 Du, Parise, Müller Ident. Title of Investigation Authors 191-09 Deuteration in the massive dense cores of Cygnus X Bontemps, Herpin, Jacq, Csengeri, Schneider, Motte, Gallardo Annual report 2010 41 Ident. Title of Investigation Authors 192-09 Tracing gas accretion in galactic nuclei using the Riquelme, Amo Baladrón, Martín-Pintado, Mauersberger, Martín isotopic ratios 193-09 The relation between evolution and deuteration in Fontani, Caselli, Jimenez-Serra, Tan, Butler, Leurini, Audard, Busquet, Estalella, Palau, Sanchez-Monge massive star formation 198-09 The CMF as an age tracer: Relative deuteration in Rodón, Beuther, Schilke, Zhang MSF regions 199-09 Hunting for molecules in proto-planetary disks Fuente, Cernicharo, Goicoechea, Alonso-Albi, Berné, Agúndez (PPDs) 200-09 Sulfur during Planetary System For-mation: Dutrey, Henning, Guilloteau, Semenov, Wakelam, Hersant, Launhardt, Pietu, Schreyer, Difolco Characterizing the Reservoir of Sulfur in Proto- planetary Disks 201-09 The Impact of Grain Evolution on Protoplanetary Guilloteau, Henning, Dutrey, Semenov, Wakelam, Launhardt, Pietu, Schreyer, Boehler disc Chemistry - The CN/HCN ratio 202-09 DCN in protoplanetary disks: the missing link Chapillon, Parise, Guilloteau between molecular clouds and comets 206-09 Characterization of debris disks around solar-type Lestrade, Phou, Bertoldi stars 207-09 Disks in the TW Hydrae Association Ducourant, Boehler, Dutrey, Guilloteau, Krone-Martins, Texeira, Galli, Chauvin, Difolco 208-09 Multiple Molecular Shells in IRC10216 Cernicharo, Agúndez, Marcelino, Guélin 209-09 A lambda 0.9 mm spectral line survey of IRC Kahane, Cernicharo, Guélin, Agúndez, Pardo +10216 211-09 Probing HBB by observations of N-bearing Alcolea, Bujarrabal, Menten, Desmurs, Jimenez-Esteban, Quintana-Lacaci molecules in CSEs: III 212-09 Metal oxides as tracers of dust condensation in De Beck, Decin, Cherchneff, Bujarrabal oxygen-rich evolved stars 215-09 CO line emission toward magnetically active AGB Ramstedt, Vlemmings, Castro-Carrizo, Maercker, Schöier, Olofsson stars 216-09 Molecular complexity in O-rich evol-ved stars: Sanchez Contreras, Alcolea, Cernicharo, Bujarrabal, Agundez, Herpin, Pardo, Menten, Wyrowsky OH₂31.8+4.2 and IK Tau 219-09 Molecular Gas in the M82 wind and cap Boulanger, Armus, Guillard, Herrera, Lehnert, Nesvadba 222-09 Tracing the Dense Gas at Large Radii in NGC 4736 Bigiel, Usero, Leroy, Walter, Blitz 223-09 Molecular Gas in the Extreme Outer Disk of M83 Bigiel, Leroy, Usero, Walter, Blitz, Madore 224-09 Probing the molecular disk-halo interface in NGC García-Burillo, Guélin, Usero, Fuente, Howk, Graciá-Carpio, Zylka 891 226-09 18O/17O as a diagnostics of star forma-tion in the Mauersberger, Henkel, Wilson, Vila-vilaró central minispiral of IC 342 228-09 A Legacy Survey to Study Cold Gas Scaling Laws in Kramer, Kauffmann, Buchbender, Catinella, Cortese, Fabello, Fu, Giovanelli, Gracia-Carpio, Guo, Haynes, the Local Universe Heckman, Krumholz, Li, Moran, Rodriguez-Fernandez, Saintonge, Schiminovich, Schuster, Sievers, Tacconi, Wang 229-09 Do Episodic Inflow Events Resupply Molecular Gas? Kannappan, Wei, Stark, Baker, Vogel 232-09 HERA 13CO(2-1) observations of the Antennae Tabatabaei, Güsten, Kramer, Requena-Torres galaxies 233-09 CO and CI Study of the ISM in Intermediate Redshift Boone, Lim, Gerin, Bayet, Papadopoulos, Trung, Matsushita ULIRGs 235-09 CO in Abell 1367: a probe for interaction Scott, Brinks, Usero, Bravo-Alfaro mechanisms 236-09 Revealing the cold gas phase in the cores of cluster Edge, Salome, Combes, Hamer, Egami of galaxies 237-09 The chemical classification of galaxies. Aladro, Martín, Riquelme, Martín-Pintado, Kramer, Güsten, Mauersberger, Weiβ, Requena-Torres, Armijos 238-09 Hot molecular gas near the AGN of NGC 1068 Mühle, Henkel, Aalto Ident. Title of Investigation Authors 242-09 The molecular gas properties of early-type galaxies Crocker, Krips, Young, Bureau, Combes, Davis, Alatalo, Blitz, Emsellem, Cappellari, Mcdermid, Krajnovic 250-09 Multiband Polarization Variability of 0716+714 and Gupta, Krichbaum, Marchili, Wiesemeyer, Thum, Fuhrmann, Nestoras, Zensus, Liu, Wiita, Gaur 0954+658 252-09 On the Road to Understanding AGN Feedback Lehnert, Boulanger, Pineau des Forêts, Guillard, Nesvadba, Appleton, Ogle 253-09 The Molecular Gas Content of the Weakest AGN Böker, Schinnerer, Lisenfeld 256-09 Coordinated cm to mm-monitoring of variability Fuhrmann, Zensus, Krichbaum, Readhead, Nestoras, Angelakis, Marchili, Ungerechts, Sievers, Riquelme and spectral evolution in Fermi blazars 257-09 Mapping a z=5 Cluster in Far-IR Emission Bremer, Stanway, Davies, Carilli, Omont, Lehnert 258-09 Search for Dust Continuum in Optically Faint Wang, Carilli, Wagg, Bertoldi, Omont, Cox, Walter, Menten, Strauss, Fan, Jiang Quasars at z~6 260-09 Further exploring starbursts down the z=6 QSO Omont, Willott, Bergeron, Delorme, Forveille, Delfosse, Cox, Beelen, Fiolet luminosity function 263-09 A MAMBO survey of the 1046+59 VLA/Herschel Omont, Baker, Beelen, Ivison, Lindner, Lonsdale, Owen, Bertoldi, Dole, Fiolet, Harris, Lutz, Polletta ultradeep field 42 Institut de Milimétrique Ident. Title of Investigation Authors 264-09 A 1.2 mm MAMBO survey of the Q1623 field Chapman, Greve, Kovacs 269-09 [CII]158um in the Early Universe: a search in a Verma, Lehnert, Tecza, Contursi, Lutz, Sturm, Schreiber z=6.17 LBG 270-09 Measuring the [CII]/CO Ratio at High Redshift Hailey-Dunsheath, Stacey, Nikola, Tacconi 271-09 Cooling at Early Times - [CII] in a Unique High Stanway, Bremer, Davies, Carilli, Omont, Lehnert Redshift Source 272-09 Search for [CII] Emission in High-z Quasars and Cox, Riechers, Walter, Carilli, Wang, Neri, Omont, Beelen, Maiolino, Menten, Wagg, Kramer, Weiss, Bertoldi Galaxies 273-09 A Comprehensive Spectral Survey of the Brightest Swinbank, Cox, Neri, Smail, Edge, Harris, Baker, Longmore, Ivison, Weiss Submillimetre Galaxy 275-09 CO redshifts of SMGs near HzRGs Weiss, Ivison, Downes, Walter, Menten 276-09 The CO line SED of J14009+0252 - evidence for a Weiss, Downes, Walter, Henkel second gas component? 277-09 Correlation between PAH and CO emission in z~1.5- Fiolet, Omont, Bertincourt, Yan, Farrah, Lagache, Lutz, Tacconi, Cox, Nesvadba, Polletta 2 Spitzer starburst ULIRGs 278-09 High-J CO Excitation in Submm-Faint Radio Galaxies Casey, Chapman, Greve, Genzel, Weiss, Tacconi, Bertoldi, Neri, Omont, Cox, Smail, Swinbank, Ivison, Blain at z~2 279-09 Search for molecular absorption at high z Combes, Bergeron, Omont, Gupta, Srianand D11-09 Improve Spectrum of NH+ in L1689B Bacmann D14-09 Search for OFF position in S140 for HERSCHEL Dedes D15-09 Finish 052-09 Goicoechea, Pety D16-09 Water Vapor in our Galaxy Cernicharo D17-09 Master Students Training LeBourlot D19-09 Short-spacings CO map to correct a complex Van Loon, Davies, Messineo, Kastner, Figer Plateau de Bure CO map D20-09 MAMBO snapshots: Obtaining the flux at 1.2mm of Dannerbauer, Omont, Bertoldi, Beelen, Negrello, Verma, strong gravitational lens candidates selected in the Herschel-ATLAS SDP field D21-09 DDT: The SiO masers of the recent nova V407 Cyg Vlemmings, Fuhrmann, Humphreys, Ramstedt, Maercker D22-09 DDT observations of comet 29P/Schwassmann- Bockelée-Morvan, Biver, Crovisier, Lellouch, Colom, Moreno, Hartogh, Lis, Boissier, Paubert Wachmann in support of Herschel 001-10 Jupiter’s atmosphere 16 years after SL9 impact Moreno, Marten, Paubert Ident. Title of Investigation Authors 002-10 The composition of Jupiter-family comet 10P/ Crovisier, Biver, Bockelée-Morvan, Colom, Moreno, Hartogh, Lis, Boissier, Paubert, Weaver, Russo, Vervack Tempel 2 003-10 A Close-up Look at Comet 103P/Hartley 2 Drahus, Jewitt, Thum, Sievers, Guilbert, Waniak, Bonev, Borisov 004-10 Understanding the composition of Earth-grazing Biver, Crovisier, Bockelée-Morvan, Colom, Moreno, Hartogh, Lis, Boissier, Paubert, Weaver, Russo, Vervack comet 103P/Hartley 2 005-10 Dense gas from an excellent proto brown dwarf Palau, de Gregorio-Monsalvo, Morata, Huelamo, Barrado y Navascués candidate 011-10 Unbiased cens of Cores in the Pipe Nebula Bowl’s Frau, Girart, Beltrán, Morata, Alves, Franco, Busquet, Estalella, Masqué, Sánchez-Monge, Padovani center 012-10 Cloud Core Structure from Observations of C18O Pagani, Goldmsith, Liseau, Li, De Luca, Bell 015-10 Tracing Dense Gas in IRDCs: A Prelude to Herschel, Linz, Schmiedeke, Pavlyuchenkov, Krause, Henning Act II 016-10 A search for indications of small-scale clumpiness in Pirogov, Zinchenko massive cores 017-10 A study of W40 pre-protostellar dense core Pirogov, Wu, Zhu 018-10 Tracing dust temperatures and co-lumn density: Stutz, Launhardt, Henning, Kainulainen, Krause, Linz, Nielbock, Schmalzl, Steinacker from Herschel to IRAM 020-10 Fragmentation of Young Filaments within Hacar, Kainulainen, Tafalla, Beuther, Qintana-Lacaci Molecular Clouds 021-10 Assembling molecular clouds: mm continuum and Beuther, Kainulainen NIR extinction 024-10 Large scale kinematics of two Herschel filaments Peretto, André, Maury, Menshchikov, Konyves, Bontemps, Didelon, Attard in Aquila 025-10 The Transition to Coherence in Dense Cores: B5 as Pineda, Jimenez-Serra, Schnee, Caselli, Goodman, Arce, Tafalla, Hacar a test 026-10 Sequential star-formation in Isolated Dark Clouds Schmalzl, Launhardt, Bourke, Stutz, Henning - A kinematic study of the Bok globule CB 130 029-10 Examining the Role of Magnetic Fields in Starless Lee, Looney, Raab, Mouschovias, Kunz Cores Annual report 2010 43 Ident. Title of Investigation Authors 030-10 The magnetic precursor of C-type shocks in young Roberts, Jiménez-Serra, Gusdorf, Martín-Pintado, Rodríguez-franco, Viti molecular outflows 033-10 Comparison of turbulence in two nearby molecular Hily-Blant, Falgarone, Hennebelle, Lesaffre clouds 034-10 CH3OH masers and the magnetic field in the central Wiesemeyer, Strelnitski, Pratap, Thum molecular zone 035-10 Magnetic field diagnostics in MSX IR dark clouds: 1. Poidevin, Wiesemeyer, Bastien, Vastel A search for Zeeman tracers in CL04 037-10 A High Sensitivity Search for Millime-ter Radio Schuster, Sterzik, Lefloch, Thum, Guedel Recombination Lines around YSO’s 038-10 On the chemical effects of the propagation of a Amo Baladrón, Armijos, Riquelme, Martín-Pintado, Terrier, Ponti, Goldwurm X-ray wave front through the GMCs of the GC. 042-10 The chemical structure of Orion : Completion of the Marcelino, Cernicharo, Bañó, Palau, Tercero, Guélin 2-D line survey at 1mm 043-10 Search for complex molecules in the Serpens core Kristensen, Öberg, Visser, Isokoski, Dishoeck 045-10 Ionization of cosmic-ray irradiated molecular clouds Montmerle, Ceccarelli, Dubus, Hily-Blant, Lefloch, Fiasson, Gallant, Gabici, Elitzur near the SNR W28 046-10 Investigating the nitrogen isotopic fractionation Bizzocchi, Caselli, Dore mechanism in cold quiescent clouds: a search for 15 + 15 + N2H and N ND in L1544 049-10 Dilution of the 13C Isotopic Species in Dark Cloud Yamamoto, Sakai, Sakai 050-10 Production of amino acids in the Perseus molecular Iglesias-Groth, Gómez, Manchado complex? Ident. Title of Investigation Authors 051-10 Search for medium-size anions in molecular sources Agúndez, Cernicharo, Guélin, Marcelino, Roueff, Mccarthy, Thaddeus 052-10 Chemical complexity in strongly UV-illuminated Goicoechea, Fuente, Cernicharo, Bañó, Marcelino, García-Burillo, Usero regions: 2 mm 054-10 Tracing gas accretion in Galactic nuclei using the Riquelme, Amo Baladrón, Martín-Pintado, Mauersberger, Martín isotopic ratios 055-10 The relation between evolution and deuteration in Fontani, Caselli, Jimenez-Serra, Tan, Butler, Leurini, Audard, Busquet, Estalella, Palau, Sanchez-Monge massive star formation 056-10 Selective deuteration of methanol in Ratajczak, Faure, Kahane, Ceccarelli, Taquet, Quirico, Pacheco, Lefloch protostars 061-10 Search of CH₂D+: a test of gas phase deuteration in Roueff, Gerin, Lis, Wootten, Black, Guélin, Cernicharo, Marcelino warm environments 062-10 Initial Conditions of High-Mass Star Formation Tackenberg, Henning, Beuther 063-10 The molecular counterpart to HH jets from A stars Alonso-Albi, Bachiller, Ginard, Fuente 065-10 The interaction of molecular outflows and HII Gerin, Falgarone, De Luca, Godard, Lesaffre, Cabrit, Lis, Menten, Mookerjea, Bell, Black, Vastel, Coutens regions massive star forming regions 068-10 A new pathfinder for water in warm proto- Ceccarelli, Cernicharo planetary disks 069-10 DCN in protoplanetary disks: the missing link Chapillon, Parise, Guilloteau between molecular clouds and comets 070-10 Tracing X-ray/UV irradiation of proto-planetary disks Semenov, Guilloteau, Dutrey, Boehler, Chapillon, Gueth, Henning, Hersant, Launhardt, Pietu, Schreyer, with ethynyl radical Wakelam 072-10 Spatially resolving an extended debris disk around a Lestrade, Phou, Lassus nearby solar-type star 073-10 Further observations of molecular emission from Bujarrabal, Ajewska, Alcolea, Quintana-Lacaci the symbiotic star RAqr 074-10 Excited H₂O in M-type Asymptotic Giant Branch Maercker, Menten, Olofsson, Ramstedt, Schöier stars 075-10 Thermal Emission from Colliding Winds in Wolf- Montes, Rodriguez, Perez-Torres, Alberdi Rayet Stars 076-10 CO line emission toward magnetically active AGB Ramstedt, Vlemmings, Castro-Carrizo, De Lima-leal-Ferreira, Maercker, Olofsson, Schöier stars 078-10 CO observations near the bow-shock in IRC+10216 Groenewegen 079-10 Unveiling the rich chemistry of yellow hypergiant Quintana-Lacaci, Bujarrabal, Castro-Carrizo, Sánchez-Contreras, Alcolea stars: IRC+10420 081-10 Confirmation and excitation of CO and13 CO in Rizzo, Gómez, Osorio, Suárez, Miranda water fountain stars 082-10 Study of the characteristics of the CSEs around Red Quintana-Lacaci, Bujarrabal, Alcolea, Castro-Carrizo supergiant stars 083-10 High-Velocity Outflows in AGB Binaries discovered Sahai, Contreras, Findeisen, Gil De Paz with GALEX 085-10 A complete and deep HERA map of M33 Braine, Schuster, Rodriguez, Kramer, Sievers, Gratier, Brouillet, Herpin, Bontemps, Israel, Van Der Werf, van der Tak, Tabatabaei, Henkel, Roellig, Combes, Wiedner, García-Burillo, Aalto, Xilouris, Wiklind, Mookerjea, Koribalski, Calzetti, Corbelli 44 Institut de Milimétrique Ident. Title of Investigation Authors 086-10 The origin of the thick molecular disk of NGC 891 García-Burillo, Guélin, Usero, Fuente, Howk, Graciá-Carpio, Zylka 088-10 The Star Formation - Molecular Gas Connection in Watson, Martini, Böker, Gil De Paz, Lisenfeld, Schinnerer an Extended UV Disk 089-10 HERA (13)CO(2-1) observations of the Antennae Tabatabaei, Güsten, Kramer, Requena galaxies 090-10 18O/17O as a diagnostics of star forma-tion in the Mauersberger, Aladro, Henkel, Wilson, Vila-vilaró central minispiral of IC 342 092-10 Molecules and dust in HeViCS galaxies Corbelli, Bianchi, Giovanardi, Magrini, Clemens, Gavazzi, Hunt, Sabatini, Baes, Delooze, Verstappen, Fritz, Garcia-Appadoo, Boselli, Jones, Madden, Bomans, Pierini, Zibetti, Xilouris, Grossi, Vlahakis, Davies, Cortese, Hughes, Bendo, Dariush, Pohlen, Smith, Fadda 094-10 CO Line Ratios and Physical Conditions in the Rosolowsky, Weiss, Usero, Leroy, Walter, Schuster, Israel HERACLES Sample 095-10 Gas consumption and expulsion in starbursts Wild, Nesvadba, Lehnert 097-10 Carbon monoxide in low-metallicity starbursts Hunt, García-Burillo, Caselli, Combes, Bovinelli, Maiolino, Menten, Weiss 098-10 Studying the dust properties in starbursting dwarf Lisenfeld, Relaño, Hermelo, Fischera galaxies 099-10 Molecular Gas Observations of Luminous Infrared Iwasawa, Evans, Aalto, Frayer, Surace, Privon, Kim, Mazzarella, Armus Galaxies in the Great Observatories All-sky LIRG Survey (GOALS) 100-10 Molecular clouds in the hot intracluster medium: Combes, Salomé, Braine Virgo 103-10 Understanding the densest molecular gas Bayet, Viti, Martín-Pintado, Martín, Aladro component in external galaxies 104-10 The chemical classification of galaxies. Aladro, Martín, Riquelme, Martín-Pintado, Kramer, Güsten, Mauersberger, Weiβ, Requena-Torres, Armijos 105-10 Excitation of Dense Molecular Gas in Galaxy Nuclei Israel, Meijerink, Loenen 108-10 Densitometry and Thermometry of Starburst Menten, Henkel, Mangum, Darling Galaxies 109-10 The extraordinary conditions of the molecular gas Rodríguez, Aalto, Mühle, Odriozola, Pérez Torres, Costagliola in nearby active galaxies 110-10 A Dedicated Line Survey of Mrk 231 Henkel, Van Der Werf, Weiβ, Martín-Pintado, Aalto, Aladro, Roberts, Gonzalez-Alonso 112-10 Cold dust along the major axis of the spiral galaxy Quintana-Lacaci, Kramer, Sievers, Buchbender, Tabatabaei, Akras, Xilouris, Aalto, Braine, Bertoldi, Van Der M33 - the HERM33S project. Werf, Wiedner 113-10 The First 3 mm Polarimetric Survey of a Complete Agudo, Thum, Wiesemeyer, Marscher, Jorstad, Gómez Sample of Blazars 115-10 Hot molecular gas near the AGN of NGC 1068 Mühle, Henkel, Aalto 116-10 Coordinated cm to mm-monitoring of variability Fuhrmann, Zensus, Nestoras, Krichbaum, Angelakis, Marchili, Ungerechts, Sievers, Riquelme, Readhead and spectral shape evolution of a selected Fermi blazar sample 118-10 Dust in Radio-Loud Broad Absorption Line Quasars Bruni, Mack, Salerno, Montenegro Montes, Carballo, Gonzalez-Serrano, Holt, Benn, Lujan 119-10 Molecular gas in a complete sample of young radio Orienti, Mack, Dallacasa sources 121-10 A Fairly Short Proposal to Observe a Very Interesting Baker, Shin, Strauss Object 122-10 Detecting dust continuum in two massive star Karim, Schinnerer, Carilli, Bertoldi, Capak, Michalowski forming galaxies at z>4 124-10 Dust emission from lensed galaxies within and after Boone, Schaerer, Pelló, Combes, Dessauges-Zavadsky, Semelin the Epoch of Reionization 128-10 Understanding the Lack of a [CII] Deficit at z~1 Hailey-Dunsheath, Stacey, Nikola, Tacconi 133-10 CO in Intermediate Redshift ULIRGs Boone, Lim, Gerin, Bayet, Papadopoulos, Trung, Matsushita 135-10 The search of molecular gas absorption at high-z Petitjean, Srianand, Gupta, Combes, Noterdaeme, Ledoux, Vergani 136-10 The brightest SMG in the North? – The EMIR view Lestrade, Salomé, Combes, Omont, Bertoldi, André, Schneider 137-10 MAMBO observations of the most luminous Perez-Fournon, Omont, Isaak, Daddi, Ferrero, Castro-Rodriguez, Cava, Martín-Pintado, Elbaz, Herschel sources Burgarella, Ivison, Clements, Oliver, Rigopoulou, Dowell Plateau de Bure Interferometer Ident. Title of Investigation Authors OF4E Deep study of the circumstellar envelo-pes of AGB & Castro-Carrizo, Alcolea, Bujarrabal, Grewing, Lucas, Neri, Oloffson, Schöier, Winters, Lindqvist early post-AGB stars R06D Dynamical disk perturbations in high accretion T Cabrit, Pety, Dougados, Beust Tauri stars R073 Disk Masses of the rho-Oph Brown Dwarfs Natta, Testi, Neri R0AB Fuelling and Feedback in the Nucleus of NGC1068 Davies, Tacconi, Combes, Baker, Schinnerer, Hicks, Genzel, Sanchez R0E7 Ionized Carbon in High-Redshift QSOs Bertoldi, Walter, Kurk, Carilli, Wagg, Aravena, Maiolino, Cox, Neri, Omont, Menten, Weiss Annual report 2010 45 Ident. Title of Investigation Authors S042 The SED of the Cloverleaf at mm wavelengths: a key Guélin, Neri, Salomé, Cox, Winters, Zylka to the dust and gas properties in the circumnuclear ring S07B Tracing ionization structure of proto-planetary disks Semenov, Guilloteau, Henning, Dutrey, Chapillon, Gueth, Hersant, Launhardt, Pavlyuchenkov, Pietu, Schreyer, Wakelam S081 The spiral features around the Herbig Ae star AB Guilloteau, Tang, Ho, Ohashi, Piétu, Dutrey Auriga S0D7 Star Forming Histories and Gas Fractions of Galaxies Genzel, Tacconi, Davis, Bolatto, Bournaud, Burkert, Combes, Cooper, Cox, Schreiber, Garcia-Burillo, Gracia- from z=1-3 Carpio, Lutz, Naab, Neri, Omont, Shapiro, Shapley, Sternberg, Weiner T--1 CII 158 micron line toward the z=6.23 QSO Bertoldi, Neri, Cox, Carilli, Walter, Wang J1048+4637 T--4 Climbing the ladder from the bottom up: mid-J CO Sharon, Baker, Harris, Tacconi, Lutz lines in SMM00266+1708 T--5 Spectral variations during flaring activity at Massi, Menten, Loinard, Kerp, Torricelli-Ciampioni, Neidhöfer, Torres periastron passage of V773TauA T--6 1.2mm imaging of strong gravitational lens Omont, Bertoldi, Beelen, Dannerbauer, Negrello, Neri, Cox candidates selected in the Herschel-ATLAS SDP field T--7 H recombination lines in LKHA101 Thum T--8 CH3CN in G29.96-0.02 Fontani T--9 CO(7-6) and CI in the Eyelash Cox, Neri, Krips T--A CO(1-2) in Pluto Bremer T--B HCOP and HCN in CRL618 Castro-Carrizo T--C CO isotopes in M82 Guélin T--D CO detection of strong gravitational lens candidates Omont, Bertoldi, Beelen, Dannerbauer, Negrello, Neri, Cox selected in the Herschel-ATLAS SDP field T--E CO detection of strong gravitational lens candidates Omont, Bertoldi, Beelen, Dannerbauer, Negrello, Neri, Cox selected in the Herschel-ATLAS SDP field T--F Molecular Gas in the Most Distant Submm Galaxy Riechers, Capak, Carilli, Schinnerer, Bertoldi, Cox, Neri, Scoville, Yan and its Environment at z=5.3 T--G Search for redshifted hydrogen fluoride in Lis, Phillips, Gerin, Neufeld, Cox, Neri APM08279+5255 T--H [CII] in a GRB host galaxy at z=8.26 Walter, Bertoldi, Carilli, Cox, Greve, Neri, Riechers, Weiss T--I Blind CO detection at 3mm in ATLAS15-141 Cox, Krips T01F The nature of the C-rich evolved stars with high Quintana-Lacaci, Bujarrabal, Castro-Carrizo circumstellar expansion velocity T031 Molecular gas in type-2 quasars at z~0.1-0.4: Testing Krips, Neri, Cox type-2/type-1 unification models T04D Atomic carbon in high-redshift quasars Knudsen, Bertoldi, Cox, Omont, Fiolet, Carilli, Riechers T057 M51: A Unique Laboratory to Study the Evolutionary Schinnerer, Leroy, Rix, Dumas, Kramer, Schuster, Thompson, Garcia-Burillo, Pety, Meidt Sequence of GMCs T058 Mapping the D/H ratio in the Martian atmosphere Fouchet, Moreno, Lellouch, Montmessin T05C Physical modeling of the supersonically contracting Masqué, Girart, Estalella, Beltrán, Osorio, Anglada star forming core ahead of HH80N T05D Origin of Water in Low-Mass Protostars Jorgensen, Lindberg, Dishoeck T05F Probing the formation of binary stars: A survey of André, Maury, Gueth, Hennebelle, Cabrit, Bate, Stamatellos, Duchêne, Bouvier, Belloche, Bontemps, Motte Class 0 objects T062 Completing the study of the proto-cluster IC 1396-N Fuente, Alonso-Albi, Beltran, Castro-Carrizo, Ceccarelli, Codella, Lefloch, Neri T064 Kinematics of massive protostars in their earliest Csengeri, Schneider, Motte, André, Bontemps, Herpin, Gueth, Hennebelle stage of evolution T065 Properties of clusters forming around massive Palau, Fuente, Busquet, Zhang, Neri, Sánchez-Monge, Boissier, Pietu, Estalella, Fontani, Audard, Alonso-Albi, protostars Ho, Zapata T077 X-ray/mm Monitoring of Colliding Magnetospheres Salter, Getman, Hogerheijde, Blake, Wilner T078 Origin of High-velocity CO in DG Tau Codella, Cabrit, Guedel, Gueth, Cesaroni, Dougados T07B The structure of the ``Butterfly Star’s’’ famous edge- Sauter, Wolf, Dutrey, Guilloteau, Boehler on disc with high resolution T083 Exploration of the architecture of the planetary Moór, Ábrahám, Csengeri, Kiss, Kóspál, Mosoni, Sándor system around HR 8799 T089 Unvealing the interaction between the molecular Castro-Carrizo, Contreras, Bujarrabal, Neri, Alcolea gas and extremely fast winds in the PPNe M 2-56 T08C Molecular Clouds and Stellar Feedback in NGC 2403 Leroy, Schinnerer, Rosolowsky, Bolatto T093 Dust grain disruption in NGC 1068 through SiO Usero, García-Burillo, Fuente, Graciá-Carpio, Krips, Planesas, Neri emission: radiation- or shock-driven? T09C Probing extreme AGN feedback in radio galaxies Garcia-Burillo, Combes, Usero, Morganti, Soria-Ruiz, Fuente, Oosterloo, Neri T0A1 Testing the mechanism of bulge growth in cluster Geach, Smail, Bower, Edge starbursts: where is the gas? 46 Institut de Milimétrique Ident. Title of Investigation Authors T0A3 Cross-calibrating masses of quasar host galaxies Jahnke, Walter, Riechers T0A4 The CO Morphology of a High-Redshift Galaxy Hailey-Dunsheath, Stacey, Nikola, Tacconi Detected in [CII] T0AA High-resolution Observations of CO in the Brightest Cox, Swinbank, Neri, Krips, Smail, Edge, Harris, Baker, Longmore, Ivison, Weiss Submillimetre Galaxy T0AB High-resolution mapping of a lensed UV-selected Baker, Lutz, Tacconi, Lin, Allam, Tucker, Shapley, Diehl star-forming galaxy T0AD Characterising the molecular gas in a high-redshift Martinez-Sansigre, Lacy, Schinnerer, Rawlings obscured quasar T0AF A Systematic Study of CO Excitation in High-Redshift Riechers, Walter, Carilli, Neri, Cox, Weiss, Bertoldi Quasar Host Galaxies T0B2 Where are the sites of active star formation in the Dannerbauer, Walter, Tapken, Yang, Matsuda, Yamada, Hayashino Lyα blob LAB1? T0B5 Unveiling a population of massive dust-enshrouded Cirasuolo, Dannerbauer, Ivison, Greve, Dunlop, McLure, Daddi galaxies at z>3 T0B7 The Spatially Resolved Star Formation Law in Riechers, Daddi, Carilli, Walter, Morrison, Krips, Dannerbauer, Elbaz Clustered z>4 Submm Galaxies T0BA Molecular gas and dust in an extreme star forming Schinnerer, Carilli, Smolvcic, Capak, Bertoldi galaxy in the young universe T0C4 Ionized Carbon in High-Redshift QSOs Bertoldi, Walter, Knudsen, Carilli, Wang, Neri, Maiolino, Cox, Omont, Menten, Weiss, Aravena, Wagg, Riechers, Kurk T0C5 The [CII]-forest: a new powerful tool for cosmology Maiolino, Gallerani, Ferrara, Lutz, Genzel, Tacconi T0C6 [CII] Emission in Actively Starforming Galaxies at Walter, Carilli, Riechers, Bertoldi, Cox, Neri, Weiss, Wagg, Ouchi, Egami, Iono, Nakanishi Redshifts ~6.5-7.0 T0C7 [CII] in a GRB host galaxy at z=8.26 Walter, Bertoldi, Carilli, Cox, Greve, Neri, Riechers, Weiss T0C8 Millimetre observations of GRB afterglows in the it Castro-Tirado, Bremer, Winters, Gorosabel, Guziy, De Ugarte Postigo, Pérez-Ramírez, Jelinek, Kubánek Swift and it Fermi era (ToO) T0C9 The Polarization of Sgr A* on a 25 Schwarzschild Krichbaum, Trippe, Bremer, Wiesemeyer, Lu, Graham, Roy, Alef, Zensus Radii Scale T0CC IRAM Lensing Survey: Probing Galaxy Formation in Kneib, Clément, Cuby, Peroux, Ilbert, Jablonka, Boone, Combes, Neri, Krips, Lagache, Beelen, Pello, Courbin, the Early Universe Meylan, Schaerer, Dessauges, Knudsen, Van der Werf, Richard, Smail, Swinbank, Chapman, Ivison, Egami, Altieri, Valtchanov U--1 Multi-line CO snapshot of the brightest HerMES Omont, Neri, Beelen, Krips, Perez-Fournon, Gavazzi, Cooray, Bock, Clements, Dowell, Ivison, Lupu, Vieira lensed SMG at z=2.95 U--2 Detecting stellar outflow feedback in a spectacular Genzel, Tacconi rotating-clump cluster galaxy U--3 Multi-line CO snapshots of Three Bright HerMES Fiolet, Omont, Beelen, Krips, Perez-Fournon, Aussel, Dannerbauer, Cooray, Riechers, The Hermes Consortium lensed SMGs U--5 Molecular filament in the Crab Nebula Salome, Hily-Blant, Castro-Carrizo, Ferland, Combes, Baldwin, Loh U--6 Bright CO(5-4) from a lensed SMG at redshift 5.7 Omont, Cooray, Riechers, Cox, Krips, Neri U001 Imaging the inner coma of comet 103P/Hartley 2 Boissier, Bockelée-Morvan, Biver, Crovisier, Moreno, Colom, Groussin, Jorda, Lamy U002 Absorption line clouds toward SgrB2 Schilke, Lis, Qin, Rolffs, Comito, Belloche, Menten U003 Methyl formate and methanol: two key complex Taquet, Ceccarelli, Kahane, Neri, Ratajczak, Faure, Lefloch, Pacheco, Bacmann, Quirico, Wiesenfeld, Szalewicz organic molecules U009 Studying Low Mass Star Formation Within a Dense Trippe, Brown, Brown, Eriksson Filament in Serpens U00B The relation between deuteration and evolution in Fontani, Gueth, Caselli, Tan, Butler, Jimenez-Serra, Busquet, Palau, Sanchez-Monge massive star formation U00D Connecting massive embedded protostars on their Ragan, Beuther, Henning, Linz natal IRDC U00F The protostellar population in the IR-dark ``tail” in Beltrán, Fontani, Codella, Massi, López IC 1396N U010 Unveiling the kinematics of the ionized jet in Jimenez-Serra, Martin-Pintado, Thum, Patel Cepheus A HW2 U011 The Impact of Grain Evolution on Protoplanetary Guilloteau, Henning, Dutrey, Chapillon, Semenov, Wakelam, Launhardt, Pietu, Schreyer, Boehler, Hincelin Disc Chemistry: The CN/HCN ratio U019 Testing the Anion Chemistry in IRC+10216 Guélin, Cernicharo, Agundez, Winters, Thaddeus, Mccarthy U01E Measuring the dynamics of a Tidal Dwarf Galaxy: Lisenfeld, Duc, Brinks, Charmandaris, Braine, Bournaud insight on the missing baryons U020 Shock and star formation in the Stephan’s Quintet Guillard, Boulanger, Duc, Appleton, Cluver, Falgarone, Lisenfeld, Ogle, Pineau des Forêts galaxy collision U021 The Disk-Starburst Transition in the Centers of Walter, Leroy, Bigiel, Sandstrom, Bolatto, Weiss, Schuster HERACLES Galaxies U026 The physics of AGN feedback in Mrk231 Feruglio, Fiore, Maiolino, Piconcelli, Aussel, Lamastra U02A Revealing the quasar feedback through broad CO Maiolino, Feruglio, Fiore, Piconcelli, Neri lines Annual report 2010 47 Ident. Title of Investigation Authors U030 The Dense Star-Forming Interstellar Medium in Riechers, Walter, Carilli, Daddi, Dannerbauer, Cox `Normal’ High Redshift Galaxies U031 The z=1 Star Formation Law with Herschel and IRAM Saintonge, Lutz, Magnelli, Berta, Tacconi, Genzel, Nordon, Popesso, Schreiber, Rodighiero, Maiolino U034 Understanding the Origins of [CII] Emission in z~1 Hailey-Dunsheath, Stacey, Nikola, Tacconi Quasars U036 A pilot study of the molecular gas in cluster ULIRGs Pope, Armus, Brodwin, Bussmann, Desai, Dey, Jannuzi, Le Floc’h, Melbourne, Soifer at z>1 U038 CO excitation conditions in 1 Annex II PUBLICATIONS IN 2010 The list of refereed publications, conference and workshop papers as well as thesis based upon data obtained using the IRAM instruments are provided in the following two tables: the first table gives the publications with the IRAM staff members as (c0)-author (including technical publications by the IRAM staff) and the second table those with results from the user’s community. The running number is the cumulative number since the first annual report was published for the year 1987. 2010 publication list: IRAM community 1472 The molecular gas content of the advanced Jütte E., Aalto S., Hüttemeister S. A&A 509, A19 S+E merger NGC 4441. Evidence for an extended decoupled nuclear disc? 1473 Detection of N15NH+ in L1544 Bizzocchi L., Caselli P., Dore L. A&A 510, L5 1474 A rotating molecular jet in Orion Zapata L. A., Schmid-Burgk J., Muders D., Schilke P., Menten K., Guesten R. A&A 510, A2 1475 Three intermediate-mass young stellar Palau A., Sánchez-Monge Á., Busquet G., Estalella R., Zhang Q., Ho P. T. P., Beltrán M. T., Beuther H. A&A 510, A5 objects with different properties emerging from the same natal cloud in IRAS 00117+6412 1476 A multi-wavelength study of the young star Audard M., Stringfellow G. S., Güdel M., Skinner S. L., Walter F. M., Guinan E. F., Hamilton R. T., Briggs A&A 511, A63 V1118 Orionis in outburst K. R., Baldovin-Saavedra C. 1477 L1506: a prestellar core in the making Pagani L., Ristorcelli I., Boudet N., Giard M., Abergel A., Bernard J.-P. A&A 512, A3 1478 Abundance anomaly of the 13C species of Sakai N., Saruwatari O., Sakai T., Takano S., Yamamoto S. A&A 512, A31 CCH 1479 Toward understanding the formation of Maury A. J., André P., Hennebelle P., Motte F., Stamatellos D., Bate M., Belloche A., Duchêne G., A&A 512, A40 multiple systems. A pilot IRAM-PdBI survey of Whitworth A. Class 0 objects 1480 Nitrogen chemistry and depletion in starless Hily-Blant P., Walmsley M., Pineau Des Forêts G., Flower D. A&A 513, A41 cores 1481 Initial phases of massive star formation in Rygl K. L. J., Wyrowski F., Schuller F., Menten K. M. A&A 515, A42 high infrared extinction clouds *. I. Physical parameters 1482 Vibrationally excited HC3N in NGC 4418 Costagliola F., Aalto S. A&A 515, A71 1483 Circumstellar molecular composition of the Decin L., de Beck E., Brünken S., Müller H. S. P., Menten K. M., Kim H., Willacy K., de Koter A., Wyrowski A&A 516, A69 oxygen-rich AGB star IK Tauri. II. In-depth F. non-LTE chemical abundance analysis 1484 Physical structure of the envelopes of Crimier N., Ceccarelli C., Alonso-Albi T., Fuente A., Caselli P., Johnstone D., Kahane C., Lefloch B., Maret A&A 516, A102 intermediate-mass protostars S., Plume R., Rizzo J. R., Tafalla M., van Dishoeck E., Wyrowski F. 1485 The puzzling behavior of HNCO isomers in Marcelino N., Brünken S., Cernicharo J., Quan D., Roueff E., Herbst E., Thaddeus P. A&A 516, A105 molecular clouds 1486 Interstellar HOCN in the Galactic center Brünken S., Belloche A., Martìn S., Verheyen L., Menten K. M. A&A 516, A109 region 1487 The NHD/NH ratio toward pre-protostellar Busquet G., Palau A., Estalella R., Girart J. M., Sánchez-Monge Á., Viti S., Ho P. T. P., Zhang Q. A&A 517, L6 cores around the UC H II region in IRAS 20293+3952 1488 TIMASSS: the IRAS16293-2422 millimeter Demyk K., Bottinelli S., Caux E., Vastel C., Ceccarelli C., Kahane C., Castets A. A&A 517, A17 and submillimeter spectral survey: tentative detection of deuterated methyl formate (DCOOCH3) 1489 A comparative study of high-mass cluster López-Sepulcre A., Cesaroni R., Walmsley C. M. A&A 517, A66 forming clumps 1490 A line confusion limited millimeter survey of Tercero B., Cernicharo J., Pardo J. R., Goicoechea J. R. A&A 517, A96 Orion KL . I. Sulfur carbon chains 1491 Herschel ATLAS: The cosmic star formation Serjeant S., Bertoldi F., Blain A. W., Clements D. L., Cooray A., Danese L., Dunlop J., Dunne L., Eales S., A&A 518, L7 history of quasar host galaxies Falder J., Hatziminaoglou E., Hughes D. H., Ibar E., Jarvis M. J., Lawrence A., Lee M. G., MichaŃowski M., Negrello M., Omont A., Page M., Pearson C., van der Werf P. P., White G., Amblard A., Auld R., Baes M., Bonfield D. G., Burgarella D., Buttiglione S., Cava A., Dariush A., de Zotti G., Dye S., Frayer D., Fritz J., Gonzalez-Nuevo J., Herranz D., Ivison R. J., Lagache G., Leeuw L., Lopez-Caniego M., Maddox S., Pascale E., Pohlen M., Rigby E., Rodighiero G., Samui S., Sibthorpe B., Smith D. J. B., Temi P., Thompson M., Valtchanov I., Verma A. Annual report 2010 49 1492 The far-infrared/radio correlation as probed Ivison R. J., Magnelli B., Ibar E., Andreani P., Elbaz D., Altieri B., Amblard A., Arumugam V., Auld R., A&A 518, L31 by Herschel Aussel H., Babbedge T., Berta S., Blain A., Bock J., Bongiovanni A., Boselli A., Buat V., Burgarella D., Castro-Rodrìguez N., Cava A., Cepa J., Chanial P., Cimatti A., Cirasuolo M., Clements D. L., Conley A., Conversi L., Cooray A., Daddi E., Dominguez H., Dowell C. 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K., Combes F., Garcìa-Burillo S., Boone F., Eckart A., Neri R., Schinnerer E. A&A 510, A52 XIII. The interacting Seyfert 2/LINER galaxy NGC 5953 1392 Detection of the high z GRB 080913 and Pérez-Ramìrez D., de Ugarte Postigo A., Gorosabel J., Aloy M. A., Jóhannesson G., Guerrero M. A., A&A 510, A105 its implications on progenitors and energy Osborne J. P., Page K. L., Warwick R. S., Horváth I., Veres P., Jelìnek M., Kubánek P., Guziy S., Bremer M., extraction mechanisms Winters J. M., Riva A., Castro-Tirado A. J. 1393 H₂CO and CH3OH maps of the Orion Bar Leurini S., Parise B., Schilke P., Pety J., Rolffs R. A&A 511, A82 photodissociation region 1394 Dust properties of protoplanetary disks in Ricci L., Testi L., Natta A., Neri R., Cabrit S., Herczeg G. J. A&A 512, A15 the Taurus-Auriga star forming region from millimeter wavelengths 1395 The molecular interstellar medium of the Gratier P., Braine J., Rodriguez-Fernandez N. J., Israel F. P., Schuster K. F., Brouillet N., Gardan E. A&A 512, A68 Local Group dwarf NGC 6822. The molecular ISM of NGC 6822 1396 A millimeter survey of ultra-compact HII- Churchwell E., Sievers A., Thum C. A&A 513, A9 regions and associated molecular clouds 1397 Measurement of the Crab nebula Aumont J., Conversi L., Thum C., Wiesemeyer H., Falgarone E., Macìas-Pérez J. F., Piacentini F., A&A 514, A70 polarization at 90 GHz as a calibrator for CMB Pointecouteau E., Ponthieu N., Puget J. L., Rosset C., Tauber J. A., Tristram M. experiments 1398 The first IRAM/PdBI polarimetric millimeter Trippe S., Neri R., Krips M., Castro-Carrizo A., Bremer M., Piétu V., Fontana A. L. A&A 515, A40 survey of active galactic nuclei. I. Global properties of the sample 1399 H I and CO in the circumstellar environment Libert Y., Winters J. M., Le Bertre T., Gérard E., Matthews L. D. A&A 515, A112 of the S-type star RS Cancri 1400 CO observations of symbiotic stellar systems Bujarrabal V., MikoŃajewska J., Alcolea J., Quintana-Lacaci G. A&A 516, A19 1401 HNCO enhancement by shocks in the L1157 Rodrìguez-Fernández N. J., Tafalla M., Gueth F., Bachiller R. A&A 516, A98 molecular outflow 1402 Weak 13CO in the Cloverleaf quasar: evidence Henkel C., Downes D., Weiß A., Riechers D., Walter F. A&A 516, A111 for a young, early generation starburst 1403 Astronomical identification of CN-, the Agúndez M., Cernicharo J., Guélin M., Kahane C., Roueff E., KŃos J., Aoiz F. J., Lique F., Marcelino N., A&A 517, L2 smallest observed molecular anion Goicoechea J. R., González Garcìa M., Gottlieb C. A., McCarthy M. C., Thaddeus P. 1404 Revisiting the theory of interferometric Pety J., Rodrìguez-Fernández N. A&A 517, A12 wide-field synthesis 1405 Coordinated NIR/mm observations of flare Kunneriath D., Witzel G., Eckart A., Zamaninasab M., Gießübel R., Schödel R., Baganoff F. K., Morris A&A 517, A46 emission from Sagittarius A* M. R., Dovčiak M., Duschl W. J., Garcìa-Marìn M., Karas V., König S., Krichbaum T. P., Krips M., Lu R.-S., Mauerhan J., Moultaka J., Mužić K., Sabha N., Najarro F., Pott J.-U., Schuster K. F., Sjouwerman L. O., Straubmeier C., Thum C., Vogel S. N., Teuben P., Weiss A., Wiesemeyer H., Zensus J. A. 1406 Class I and Class II methanol masers in high- Fontani F., Cesaroni R., Furuya R. S. A&A 517, A56 mass star-forming regions Annual report 2010 53 1407 The Herschel-SPIRE instrument and its in- Griffin M. J., Abergel A., Abreu A., Ade P. A. R., André P., Augueres J.-L., Babbedge T., Bae Y., Baillie T., A&A 518, L3 flight performance Baluteau J.-P., Barlow M. J., Bendo G., Benielli D., Bock J. J., Bonhomme P., Brisbin D., Brockley-Blatt C., Caldwell M., Cara C., Castro-Rodriguez N., Cerulli R., Chanial P., Chen S., Clark E., Clements D. L., Clerc L., Coker J., Communal D., Conversi L., Cox P., Crumb D., Cunningham C., Daly F., Davis G. R., de Antoni P., Delderfield J., Devin N., di Giorgio A., Didschuns I., Dohlen K., Donati M., Dowell A., Dowell C. D., Duband L., Dumaye L., Emery R. J., Ferlet M., Ferrand D., Fontignie J., Fox M., Franceschini A., Frerking M., Fulton T., Garcia J., Gastaud R., Gear W. K., Glenn J., Goizel A., Griffin D. K., Grundy T., Guest S., Guillemet L., Hargrave P. C., Harwit M., Hastings P., Hatziminaoglou E., Herman M., Hinde B., Hristov V., Huang M., Imhof P., Isaak K. J., Israelsson U., Ivison R. J., Jennings D., Kiernan B., King K. J., Lange A. E., Latter W., Laurent G., Laurent P., Leeks S. J., Lellouch E., Levenson L., Li B., Li J., Lilienthal J., Lim T., Liu S. J., Lu N., Madden S., Mainetti G., Marliani P., McKay D., Mercier K., Molinari S., Morris H., Moseley H., Mulder J., Mur M., Naylor D. A., Nguyen H., O’Halloran B., Oliver S., Olofsson G., Olofsson H.-G., Orfei R., Page M. J., Pain I., Panuzzo P., Papageorgiou A., Parks G., Parr-Burman P., Pearce A., Pearson C., Pérez-Fournon I., Pinsard F., Pisano G., Podosek J., Pohlen M., Polehampton E. T., Pouliquen D., Rigopoulou D., Rizzo D., Roseboom I. G., Roussel H., Rowan-Robinson M., Rownd B., Saraceno P., Sauvage M., Savage R., Savini G., Sawyer E., Scharmberg C., Schmitt D., Schneider N., Schulz B., Schwartz A., Shafer R., Shupe D. L., Sibthorpe B., Sidher S., Smith A., Smith A. J., Smith D., Spencer L., Stobie B., Sudiwala R., Sukhatme K., Surace C., Stevens J. A., Swinyard B. M., Trichas M., Tourette T., Triou H., Tseng S., Tucker C., Turner A., Vaccari M., Valtchanov I., Vigroux L., Virique E., Voellmer G., Walker H., Ward R., Waskett T., Weilert M., Wesson R., White G. J., Whitehouse N., Wilson C. D., Winter B., Woodcraft A. L., Wright G. S., Xu C. K., Zavagno A., Zemcov M., Zhang L., Zonca E. 1408 The Herschel-Heterodyne Instrument for the de Graauw T., Helmich F. P., Phillips T. G., Stutzki J., Caux E., Whyborn N. D., Dieleman P., Roelfsema A&A 518, L6 Far-Infrared (HIFI) P. R., Aarts H., Assendorp R., Bachiller R., Baechtold W., Barcia A., Beintema D. A., Belitsky V., Benz A. O., Bieber R., Boogert A., Borys C., Bumble B., Caïs P., Caris M., Cerulli-Irelli P., Chattopadhyay G., Cherednichenko S., Ciechanowicz M., Coeur-Joly O., Comito C., Cros A., de Jonge A., de Lange G., Delforges B., Delorme Y., den Boggende T., Desbat J.-M., Diez-González C., di Giorgio A. M., Dubbeldam L., Edwards K., Eggens M., Erickson N., Evers J., Fich M., Finn T., Franke B., Gaier T., Gal C., Gao J. R., Gallego J.-D., Gauffre S., Gill J. J., Glenz S., Golstein H., Goulooze H., Gunsing T., Güsten R., Hartogh P., Hatch W. A., Higgins R., Honingh E. C., Huisman R., Jackson B. D., Jacobs H., Jacobs K., Jarchow C., Javadi H., Jellema W., Justen M., Karpov A., Kasemann C., Kawamura J., Keizer G., Kester D., Klapwijk T. M., Klein T., Kollberg E., Kooi J., Kooiman P.-P., Kopf B., Krause M., Krieg J.-M., Kramer C., Kruizenga B., Kuhn T., Laauwen W., Lai R., Larsson B., Leduc H. G., Leinz C., Lin R. H., Liseau R., Liu G. S., Loose A., López-Fernandez I., Lord S., Luinge W., Marston A., Martìn-Pintado J., Maestrini A., Maiwald F. W., McCoey C., Mehdi I., Megej A., Melchior M., Meinsma L., Merkel H., Michalska M., Monstein C., Moratschke D., Morris P., Muller H., Murphy J. A., Naber A., Natale E., Nowosielski W., Nuzzolo F., Olberg M., Olbrich M., Orfei R., Orleanski P., Ossenkopf V., Peacock T., Pearson J. C., Peron I., Phillip-May S., Piazzo L., Planesas P., Rataj M., Ravera L., Risacher C., Salez M., Samoska L. A., Saraceno P., Schieder R., Schlecht E., Schlöder F., Schmülling F., Schultz M., Schuster K., Siebertz O., Smit H., Szczerba R., Shipman R., Steinmetz E., Stern J. A., Stokroos M., Teipen R., Teyssier D., Tils T., Trappe N., van Baaren C., van Leeuwen B.-J., van de Stadt H., Visser H., Wildeman K. J., Wafelbakker C. K., Ward J. S., Wesselius P., Wild W., Wulff S., Wunsch H.-J., Tielens X., Zaal P., Zirath H., Zmuidzinas J., Zwart F. 1409 Black hole accretion and star formation as van der Werf P. P., Isaak K. G., Meijerink R., Spaans M., Rykala A., Fulton T., Loenen A. F., Walter F., Weiß A&A 518, L42 drivers of gas excitation and chemistry in A., Armus L., Fischer J., Israel F. P., Harris A. I., Veilleux S., Henkel C., Savini G., Lord S., Smith H. A., Markarian 231 González-Alfonso E., Naylor D., Aalto S., Charmandaris V., Dasyra K. M., Evans A., Gao Y., Greve T. R., Güsten R., Kramer C., Martìn-Pintado J., Mazzarella J., Papadopoulos P. P., Sanders D. B., Spinoglio L., Stacey G., Vlahakis C., Wiedner M. C., Xilouris E. M. 1410 Herschel observations of water vapour in González-Alfonso E., Fischer J., Isaak K., Rykala A., Savini G., Spaans M., van der Werf P., Meijerink R., A&A 518, L43 Markarian 231 Israel F. P., Loenen A. F., Vlahakis C., Smith H. A., Charmandaris V., Aalto S., Henkel C., Weiß A., Walter F., Greve T. R., Martìn-Pintado J., Naylor D. A., Spinoglio L., Veilleux S., Harris A. I., Armus L., Lord S., Mazzarella J., Xilouris E. M., Sanders D. B., Dasyra K. M., Wiedner M. C., Kramer C., Papadopoulos P. P., Stacey G. J., Evans A. S., Gao Y. 1411 PACS and SPIRE photometer maps of M 33: Kramer C., Buchbender C., Xilouris E. M., Boquien M., Braine J., Calzetti D., Lord S., Mookerjea B., A&A 518, L67 First results of the HERschel M 33 Extended Quintana-Lacaci G., Relaño M., Stacey G., Tabatabaei F. S., Verley S., Aalto S., Akras S., Albrecht M., Survey (HERM33ES) Anderl S., Beck R., Bertoldi F., Combes F., Dumke M., Garcia-Burillo S., Gonzalez M., Gratier P., Güsten R., Henkel C., Israel F. P., Koribalski B., Lundgren A., Martin-Pintado J., Röllig M., Rosolowsky E., Schuster K. F., Sheth K., Sievers A., Stutzki J., Tilanus R. P. J., van der Tak F., van der Werf P., Wiedner M. C. 1412 Properties of compact 250 mm emission and Verley S., Relaño M., Kramer C., Xilouris E. M., Boquien M., Calzetti D., Combes F., Buchbender C., A&A 518, L68 H II regions in M 33 (HERM33ES) Braine J., Quintana-Lacaci G., Tabatabaei F. S., Lord S., Israel F., Stacey G., van der Werf P. 1413 Cool gas and dust in M 33: Results from the Braine J., Gratier P., Kramer C., Xilouris E. M., Rosolowsky E., Buchbender C., Boquien M., Calzetti D., A&A 518, L69 HERschel M 33 Extended Survey (HERM33ES) Quintana-Lacaci G., Tabatabaei F., Verley S., Israel F., van der Tak F., Aalto S., Combes F., Garcia-Burillo S., Gonzalez M., Henkel C., Koribalski B., Mookerjea B., Roellig M., Schuster K. F., Relaño M., Bertoldi F., van der Werf P., Wiedner M. 1414 100 mm and 160 mm emission as resolved Boquien M., Calzetti D., Kramer C., Xilouris E. M., Bertoldi F., Braine J., Buchbender C., Combes F., Israel A&A 518, L70 star-formation rate estimators in M 33 F., Koribalski B., Lord S., Quintana-Lacaci G., Relaño M., Röllig M., Stacey G., Tabatabaei F. S., Tilanus (HERM33ES) R. P. J., van der Tak F., van der Werf P., Verley S. 1415 Initial highlights of the HOBYS key program, Motte F., Zavagno A., Bontemps S., Schneider N., Hennemann M., di Francesco J., André P., Saraceno A&A 518, L77 the Herschel imaging survey of OB young P., Griffin M., Marston A., Ward-Thompson D., White G., Minier V., Men’shchikov A., Hill T., Abergel stellar objects A., Anderson L. D., Aussel H., Balog Z., Baluteau J.-P., Bernard J.-P., Cox P., Csengeri T., Deharveng L., Didelon P., di Giorgio A.-M., Hargrave P., Huang M., Kirk J., Leeks S., Li J. Z., Martin P., Molinari S., Nguyen-Luong Q., Olofsson G., Persi P., Peretto N., Pezzuto S., Roussel H., Russeil D., Sadavoy S., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Teyssier D., Vavrek R., Wilson C. D., Woodcraft A. 1416 HIFI observations of warm gas in DR21: Ossenkopf V., Röllig M., Simon R., Schneider N., Okada Y., Stutzki J., Gerin M., Akyilmaz M., Beintema A&A 518, L79 Shock versus radiative heating D., Benz A. O., Berne O., Boulanger F., Bumble B., Coeur-Joly O., Dedes C., Diez-Gonzalez M. C., France K., Fuente A., Gallego J. D., Goicoechea J. R., Güsten R., Harris A., Higgins R., Jackson B., Jarchow C., Joblin C., Klein T., Kramer C., Lord S., Martin P., Martin-Pintado J., Mookerjea B., Neufeld D. A., Phillips T., Rizzo J. R., van der Tak F. F. S., Teyssier D., Yorke H. 1417 Physical properties of the SH₂-104 H II region Rodón J. A., Zavagno A., Baluteau J.-P., Anderson L. D., Polehampton E., Abergel A., Motte F., A&A 518, L80 as seen by Herschel Bontemps S., Ade P., André P., Arab H., Beichman C., Bernard J.-P., Blagrave K., Boulanger F., Cohen M., Compiegne M., Cox P., Dartois E., Davis G., Emery R., Fulton T., Gry C., Habart E., Halpern M., Huang M., Joblin C., Jones S. C., Kirk J., Lagache G., Lin T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Naylor D., Okumura K., Orieux F., Pinheiro Gonçalves D., Rodet T., Russeil D., Saraceno P., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. 54 Institut de Milimétrique 1418 Herschel-SPIRE spectroscopy of G29.96-0.02: Kirk J. M., Polehampton E., Anderson L. D., Baluteau J.-P., Bontemps S., Joblin C., Jones S. C., Naylor A&A 518, L82 Fitting the full SED D. A., Ward-Thompson D., White G. J., Abergel A., Ade P., André P., Arab H., Bernard J.-P., Blagrave K., Boulanger F., Cohen M., Compiegne M., Cox P., Dartois E., Davis G., Emery R., Fulton T., Gry C., Habart E., Huang M., Lagache G., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Okumura K., Pinheiro Gonçalves D., Rodón J. A., Russeil D., Saraceno P., Sidher S., Spencer L., Swinyard B., Zavagno A. 1419 The Herschel view of star formation in the Schneider N., Motte F., Bontemps S., Hennemann M., di Francesco J., André P., Zavagno A., Csengeri A&A 518, L83 Rosette molecular cloud under the influence T., Men’shchikov A., Abergel A., Baluteau J.-P., Bernard J.-P., Cox P., Didelon P., di Giorgio A.-M., Gastaud of NGC 2244 R., Griffin M., Hargrave P., Hill T., Huang M., Kirk J., Könyves V., Leeks S., Li J. Z., Marston A., Martin P., Minier V., Molinari S., Olofsson G., Panuzzo P., Persi P., Pezzuto S., Roussel H., Russeil D., Sadavoy S., Saraceno P., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Teyssier D., Vavrek R., Ward-Thompson D., White G., Wilson C. D., Woodcraft A. 1420 Herschel observations of embedded Hennemann M., Motte F., Bontemps S., Schneider N., Csengeri T., Balog Z., di Francesco J., Zavagno A&A 518, L84 protostellar clusters in the Rosette molecular A., André P., Men’shchikov A., Abergel A., Ali B., Baluteau J.-P., Bernard J.-P., Cox P., Didelon P., di Giorgio cloud A.-M., Griffin M., Hargrave P., Hill T., Horeau B., Huang M., Kirk J., Leeks S., Li J. Z., Marston A., Martin P., Molinari S., Nguyen Luong Q., Olofsson G., Persi P., Pezzuto S., Russeil D., Saraceno P., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Ward-Thompson D., White G., Wilson C., Woodcraft A. 1421 The Herschel first look at protostars in the Bontemps S., André P., Könyves V., Men’shchikov A., Schneider N., Maury A., Peretto N., Arzoumanian A&A 518, L85 Aquila rift D., Attard M., Motte F., Minier V., Didelon P., Saraceno P., Abergel A., Baluteau J.-P., Bernard J.-P., Cambrésy L., Cox P., di Francesco J., di Giorgo A. M., Griffin M., Hargrave P., Huang M., Kirk J., Li J., Martin P., Merìn B., Molinari S., Olofsson G., Pezzuto S., Prusti T., Roussel H., Russeil D., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Vavrek R., Ward-Thompson D., White G., Wilson C., Woodcraft A., Zavagno A. 1422 Small-scale structure in the Rosette di Francesco J., Sadavoy S., Motte F., Schneider N., Hennemann M., Csengeri T., Bontemps S., Balog A&A 518, L91 molecular cloud revealed by Herschel Z., Zavagno A., André P., Saraceno P., Griffin M., Men’shchikov A., Abergel A., Baluteau J.-P., Bernard J.-P., Cox P., Deharveng L., Didelon P., di Giorgio A.-M., Hargrave P., Huang M., Kirk J., Leeks S., Li J. Z., Marston A., Martin P., Minier V., Molinari S., Olofsson G., Persi P., Pezzuto S., Russeil D., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Teyssier D., Vavrek R., Ward-Thompson D., White G., Wilson C., Woodcraft A. 1423 A Herschel study of the properties of starless Ward-Thompson D., Kirk J. M., André P., Saraceno P., Didelon P., Könyves V., Schneider N., Abergel A., A&A 518, L92 cores in the Polaris Flare dark cloud region Baluteau J.-P., Bernard J.-P., Bontemps S., Cambrésy L., Cox P., di Francesco J., di Giorgio A. M., Griffin using PACS and SPIRE M., Hargrave P., Huang M., Li J. Z., Martin P., Men’shchikov A., Minier V., Molinari S., Motte F., Olofsson G., Pezzuto S., Russeil D., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., White G., Wilson C., Woodcraft A., Zavagno A. 1424 Evolution of interstellar dust with Herschel. Abergel A., Arab H., Compiègne M., Kirk J. M., Ade P., Anderson L. D., André P., Baluteau J.-P., Bernard A&A 518, L96 First results in the photodissociation regions J.-P., Blagrave K., Bontemps S., Boulanger F., Cohen M., Cox P., Dartois E., Davis G., Emery R., Fulton T., of NGC 7023 Gry C., Habart E., Huang M., Joblin C., Jones S. C., Lagache G., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Naylor D., Okumura K., Pinheiro Gonçalves D., Polehampton E., Rodon J., Russeil D., Saraceno P., Sauvage M., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. J., Zavagno A. 1425 The physical properties of the dust in the Anderson L. D., Zavagno A., Rodón J. A., Russeil D., Abergel A., Ade P., André P., Arab H., Baluteau A&A 518, L99 RCW 120 H II region as seen by Herschel J.-P., Bernard J.-P., Blagrave K., Bontemps S., Boulanger F., Cohen M., Compiègne M., Cox P., Dartois E., Davis G., Emery R., Fulton T., Gry C., Habart E., Huang M., Joblin C., Jones S. C., Kirk J. M., Lagache G., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Naylor D. A., Okumura K., Pinheiro Gonçalves D., Polehampton E., Saraceno P., Sauvage M., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. J. 1426 From filamentary clouds to prestellar cores André P., Men’shchikov A., Bontemps S., Könyves V., Motte F., Schneider N., Didelon P., Minier V., A&A 518, L102 to the stellar IMF: Initial highlights from the Saraceno P., Ward-Thompson D., di Francesco J., White G., Molinari S., Testi L., Abergel A., Griffin M., Herschel Gould Belt Survey Henning T., Royer P., Merìn B., Vavrek R., Attard M., Arzoumanian D., Wilson C. D., Ade P., Aussel H., Baluteau J.-P., Benedettini M., Bernard J.-P., Blommaert J. A. D. L., Cambrésy L., Cox P., di Giorgio A., Hargrave P., Hennemann M., Huang M., Kirk J., Krause O., Launhardt R., Leeks S., Le Pennec J., Li J. Z., Martin P. G., Maury A., Olofsson G., Omont A., Peretto N., Pezzuto S., Prusti T., Roussel H., Russeil D., Sauvage M., Sibthorpe B., Sicilia-Aguilar A., Spinoglio L., Waelkens C., Woodcraft A., Zavagno A. 1427 Filamentary structures and compact objects Men’shchikov A., André P., Didelon P., Könyves V., Schneider N., Motte F., Bontemps S., Arzoumanian A&A 518, L103 in the Aquila and Polaris clouds observed D., Attard M., Abergel A., Baluteau J.-P., Bernard J.-P., Cambrésy L., Cox P., di Francesco J., di Giorgio by Herschel A. M., Griffin M., Hargrave P., Huang M., Kirk J., Li J. Z., Martin P., Minier V., Miville-Deschênes M.-A., Molinari S., Olofsson G., Pezzuto S., Roussel H., Russeil D., Saraceno P., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Ward-Thompson D., White G., Wilson C. D., Woodcraft A., Zavagno A. 1428 Herschel-SPIRE observations of the Polaris Miville-Deschênes M.-A., Martin P. G., Abergel A., Bernard J.-P., Boulanger F., Lagache G., Anderson A&A 518, L104 flare: Structure of the diffuse interstellar L. D., André P., Arab H., Baluteau J.-P., Blagrave K., Bontemps S., Cohen M., Compiegne M., Cox P., medium at the sub-parsec scale Dartois E., Davis G., Emery R., Fulton T., Gry C., Habart E., Huang M., Joblin C., Jones S. C., Kirk J., Lim T., Madden S., Makiwa G., Menshchikov A., Molinari S., Moseley H., Motte F., Naylor D. A., Okumura K., Pinheiro Gonçalves D., Polehampton E., Rodón J. A., Russeil D., Saraceno P., Schneider N., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. J., Zavagno A. 1429 The Aquila prestellar core population Könyves V., André P., Men’shchikov A., Schneider N., Arzoumanian D., Bontemps S., Attard M., Motte A&A 518, L106 revealed by Herschel F., Didelon P., Maury A., Abergel A., Ali B., Baluteau J.-P., Bernard J.-P., Cambrésy L., Cox P., di Francesco J., di Giorgio A. M., Griffin M. J., Hargrave P., Huang M., Kirk J., Li J. Z., Martin P., Minier V., Molinari S., Olofsson G., Pezzuto S., Russeil D., Roussel H., Saraceno P., Sauvage M., Sibthorpe B., Spinoglio L., Testi L., Ward-Thompson D., White G., Wilson C. D., Woodcraft A., Zavagno A. 1430 Detection of interstellar oxidaniumyl: Ossenkopf V., Müller H. S. P., Lis D. C., Schilke P., Bell T. A., Bruderer S., Bergin E., Ceccarelli C., Comito A&A 518, L111 Abundant H₂O+ towards the star-forming C., Stutzki J., Bacman A., Baudry A., Benz A. O., Benedettini M., Berne O., Blake G., Boogert A., Bottinelli regions DR21, Sgr B2, and NGC6334 S., Boulanger F., Cabrit S., Caselli P., Caux E., Cernicharo J., Codella C., Coutens A., Crimier N., Crockett N. R., Daniel F., Demyk K., Dieleman P., Dominik C., Dubernet M. L., Emprechtinger M., Encrenaz P., Falgarone E., France K., Fuente A., Gerin M., Giesen T. F., di Giorgio A. M., Goicoechea J. R., Goldsmith P. F., Güsten R., Harris A., Helmich F., Herbst E., Hily-Blant P., Jacobs K., Jacq T., Joblin C., Johnstone D., Kahane C., Kama M., Klein T., Klotz A., Kramer C., Langer W., Lefloch B., Leinz C., Lorenzani A., Lord S. D., Maret S., Martin P. G., Martin-Pintado J., McCoey C., Melchior M., Melnick G. J., Menten K. M., Mookerjea B., Morris P., Murphy J. A., Neufeld D. A., Nisini B., Pacheco S., Pagani L., Parise B., Pearson J. C., Pérault M., Phillips T. G., Plume R., Quin S.-L., Rizzo R., Röllig M., Salez M., Saraceno P., Schlemmer S., Simon R., Schuster K., van der Tak F. F. S., Tielens A. G. G. M., Teyssier D., Trappe N., Vastel C., Viti S., Wakelam V., Walters A., Wang S., Whyborn N., van der Wiel M., Yorke H. W., Yu S., Zmuidzinas J. Annual report 2010 55 1431 The CHESS spectral survey of star forming Codella C., Lefloch B., Ceccarelli C., Cernicharo J., Caux E., Lorenzani A., Viti S., Hily-Blant P., Parise A&A 518, L112 regions: Peering into the protostellar shock B., Maret S., Nisini B., Caselli P., Cabrit S., Pagani L., Benedettini M., Boogert A., Gueth F., Melnick L1157-B1. I. Shock chemical complexity G., Neufeld D., Pacheco S., Salez M., Schuster K., Bacmann A., Baudry A., Bell T., Bergin E. A., Blake G., Bottinelli S., Castets A., Comito C., Coutens A., Crimier N., Dominik C., Demyk K., Encrenaz P., Falgarone E., Fuente A., Gerin M., Goldsmith P., Helmich F., Hennebelle P., Henning T., Herbst E., Jacq T., Kahane C., Kama M., Klotz A., Langer W., Lis D., Lord S., Pearson J., Phillips T., Saraceno P., Schilke P., Tielens X., van der Tak F., van der Wiel M., Vastel C., Wakelam V., Walters A., Wyrowski F., Yorke H., Borys C., Delorme Y., Kramer C., Larsson B., Mehdi I., Ossenkopf V., Stutzki J. 1432 The CHESS spectral survey of star forming Lefloch B., Cabrit S., Codella C., Melnick G., Cernicharo J., Caux E., Benedettini M., Boogert A., Caselli P., A&A 518, L113 regions: Peering into the protostellar shock Ceccarelli C., Gueth F., Hily-Blant P., Lorenzani A., Neufeld D., Nisini B., Pacheco S., Pagani L., Pardo J. R., L1157-B1. II. Shock dynamics Parise B., Salez M., Schuster K., Viti S., Bacmann A., Baudry A., Bell T., Bergin E. A., Blake G., Bottinelli S., Castets A., Comito C., Coutens A., Crimier N., Dominik C., Demyk K., Encrenaz P., Falgarone E., Fuente A., Gerin M., Goldsmith P., Helmich F., Hennebelle P., Henning T., Herbst E., Jacq T., Kahane C., Kama M., Klotz A., Langer W., Lis D., Lord S., Maret S., Pearson J., Phillips T., Saraceno P., Schilke P., Tielens X., van der Tak F., van der Wiel M., Vastel C., Wakelam V., Walters A., Wyrowski F., Yorke H., Bachiller R., Borys C., de Lange G., Delorme Y., Kramer C., Larsson B., Lai R., Maiwald F. W., Martin-Pintado J., Mehdi I., Ossenkopf V., Siegel P., Stutzki J., Wunsch J. H. 1433 Herschel-SPIRE spectroscopy of the DR21 White G. J., Abergel A., Spencer L., Schneider N., Naylor D. A., Anderson L. D., Joblin C., Ade P., André A&A 518, L114 molecular cloud core P., Arab H., Baluteau J.-P., Bernard J.-P., Blagrave K., Bontemps S., Boulanger F., Cohen M., Compiegne M., Cox P., Dartois E., Davis G., Emery R., Fulton T., Gom B., Griffin M., Gry C., Habart E., Huang M., Jones S., Kirk J. M., Lagache G., Leeks S., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Okumura K., Pinheiro Gonçalves D., Polehampton E., Rodet T., Rodón J. A., Russeil D., Saraceno P., Sidher S., Swinyard B. M., Ward-Thompson D., Zavagno A. 1434 SPIRE spectroscopy of the prototypical Orion Habart E., Dartois E., Abergel A., Baluteau J.-P., Naylor D., Polehampton E., Joblin C., Ade P., Anderson A&A 518, L116 Bar photodissociation region L. D., André P., Arab H., Bernard J.-P., Blagrave K., Bontemps S., Boulanger F., Cohen M., Compiegne M., Cox P., Davis G., Emery R., Fulton T., Gry C., Huang M., Jones S. C., Kirk J., Lagache G., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Okumura K., Pinheiro Gonçalves D., Rodon J., Russeil D., Saraceno P., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. J., Zavagno A. 1435 First detection of the methylidyne cation Naylor D. A., Dartois E., Habart E., Abergel A., Baluteau J.-P., Jones S. C., Polehampton E., Ade P., A&A 518, L117 (CH+) fundamental rotational line with the Anderson L. D., André P., Arab H., Bernard J.-P., Blagrave K., Bontemps S., Boulanger F., Cohen M., Herschel/SPIRE FTS Compiègne M., Cox P., Davis G., Emery R., Fulton T., Gry C., Huang M., Joblin C., Kirk J. M., Lagache G., Lim T., Madden S., Makiwa G., Martin P., Miville-Deschênes M.-A., Molinari S., Moseley H., Motte F., Okumura K., Pinheiro Gonçalves D., Rodón J. A., Russeil D., Saraceno P., Sidher S., Spencer L., Swinyard B., Ward-Thompson D., White G. J., Zavagno A. 1436 Strong CH+ J = 1-0 emission and absorption Falgarone E., Ossenkopf V., Gerin M., Lesaffre P., Godard B., Pearson J., Cabrit S., Joblin C., Benz A. O., A&A 518, L118 in DR21 Boulanger F., Fuente A., Güsten R., Harris A., Klein T., Kramer C., Lord S., Martin P., Martin-Pintado J., Neufeld D., Phillips T. G., Röllig M., Simon R., Stutzki J., van der Tak F., Teyssier D., Yorke H., Erickson N., Fich M., Jellema W., Marston A., Risacher C., Salez M., Schmülling F. 1437 Water cooling of shocks in protostellar Nisini B., Benedettini M., Codella C., Giannini T., Liseau R., Neufeld D., Tafalla M., van Dishoeck E. F., A&A 518, L120 outflows. Herschel-PACS map of L1157 Bachiller R., Baudry A., Benz A. O., Bergin E., Bjerkeli P., Blake G., Bontemps S., Braine J., Bruderer S., Caselli P., Cernicharo J., Daniel F., Encrenaz P., di Giorgio A. M., Dominik C., Doty S., Fich M., Fuente A., Goicoechea J. R., de Graauw T., Helmich F., Herczeg G., Herpin F., Hogerheijde M., Jacq T., Johnstone D., Jørgensen J., Kaufman M., Kristensen L., Larsson B., Lis D., Marseille M., McCoey C., Melnick G., Olberg M., Parise B., Pearson J., Plume R., Risacher C., Santiago J., Saraceno P., Shipman R., van Kempen T. A., Visser R., Viti S., Wampfler S., Wyrowski F., van der Tak F., Yıldız U. A., Delforge B., Desbat J., Hatch W. A., Péron I., Schieder R., Stern J. A., Teyssier D., Whyborn N. 1438 TANGO I: Interstellar medium in nearby radio Ocaña Flaquer B., Leon S., Combes F., Lim J. A&A 518, A9 galaxies. Molecular gas 1439 The CO luminosity and CO-H₂ conversion Liszt H. S., Pety J., Lucas R. A&A 518, A45 factor of diffuse ISM: does CO emission trace dense molecular gas? 1440 Extinction AV, R towards emission nebulae Greve A. A&A 518, A62 derived from common upper level Paschen- Balmer hydrogen lines 1441 [C II] line emission in BRI 1335-0417 at z = 4.4 Wagg J., Carilli C. L., Wilner D. J., Cox P., De Breuck C., Menten K., Riechers D. A., Walter F. A&A 519, L1 1442 Molecular gas chemistry in AGN. II. High- Garcìa-Burillo S., Usero A., Fuente A., Martìn-Pintado J., Boone F., Aalto S., Krips M., Neri R., Schinnerer A&A 519, A2 resolution imaging of SiO emission in NGC E., Tacconi L. J. 1068: shocks or XDR? 1443 Molecular cloud formation and the star Braine J., Gratier P., Kramer C., Schuster K. F., Tabatabaei F., Gardan E. A&A 520, A107 formation efficiency in M 33. Molecule and star formation in M 33 1444 HIFI spectroscopy of low-level water Weiß A., Requena-Torres M. A., Güsten R., Garcìa-Burillo S., Harris A. I., Israel F. P., Klein T., Kramer C., A&A 521, L1 transitions in M 82 Lord S., Martin-Pintado J., Röllig M., Stutzki J., Szczerba R., van der Werf P. P., Philipp-May S., Yorke H., Akyilmaz M., Gal C., Higgins R., Marston A., Roberts J., Schlöder F., Schultz M., Teyssier D., Whyborn N., Wunsch H. J. 1445 Excitation of the molecular gas in the Loenen A. F., van der Werf P. P., Güsten R., Meijerink R., Israel F. P., Requena-Torres M. A., Garcìa-Burillo A&A 521, L2 nuclear region of M 82 S., Harris A. I., Klein T., Kramer C., Lord S., Martìn-Pintado J., Röllig M., Stutzki J., Szczerba R., Weiß A., Philipp-May S., Yorke H., Caux E., Delforge B., Helmich F., Lorenzani A., Morris P., Philips T. G., Risacher C., Tielens A. G. G. M. 1446 Herschel/HIFI observations of high-J CO Bujarrabal V., Alcolea J., Soria-Ruiz R., Planesas P., Teyssier D., Marston A. P., Cernicharo J., Decin L., A&A 521, L3 transitions in the protoplanetary nebula Dominik C., Justtanont K., de Koter A., Melnick G., Menten K. M., Neufeld D. A., Olofsson H., Schmidt CRL 618 M., Schöier F. L., Szczerba R., Waters L. B. F. M., Quintana-Lacaci G., Güsten R., Gallego J. D., Dìez- González M. C., Barcia A., López-Fernández I., Wildeman K., Tielens A. G. G. M., Jacobs K. 56 Institut de Milimétrique 1447 Herschel/HIFI discovery of interstellar Lis D. C., Pearson J. C., Neufeld D. A., Schilke P., Müller H. S. P., Gupta H., Bell T. A., Comito C., Phillips A&A 521, L9 chloronium (H₂Cl) T. G., Bergin E. A., Ceccarelli C., Goldsmith P. F., Blake G. A., Bacmann A., Baudry A., Benedettini M., Benz A., Black J., Boogert A., Bottinelli S., Cabrit S., Caselli P., Castets A., Caux E., Cernicharo J., Codella C., Coutens A., Crimier N., Crockett N. R., Daniel F., Demyk K., Dominic C., Dubernet M.-L., Emprechtinger M., Encrenaz P., Falgarone E., Fuente A., Gerin M., Giesen T. F., Goicoechea J. R., Helmich F., Hennebelle P., Henning T., Herbst E., Hily-Blant P., Hjalmarson Å., Hollenbach D., Jack T., Joblin C., Johnstone D., Kahane C., Kama M., Kaufman M., Klotz A., Langer W. D., Larsson B., Le Bourlot J., Lefloch B., Le Petit F., Li D., Liseau R., Lord S. D., Lorenzani A., Maret S., Martin P. G., Melnick G. J., Menten K. M., Morris P., Murphy J. A., Nagy Z., Nisini B., Ossenkopf V., Pacheco S., Pagani L., Parise B., Pérault M., Plume R., Qin S.-L., Roueff E., Salez M., Sandqvist A., Saraceno P., Schlemmer S., Schuster K., Snell R., Stutzki J., Tielens A., Trappe N., van der Tak F. F. S., van der Wiel M. H. D., van Dishoeck E., Vastel C., Viti S., Wakelam V., Walters A., Wang S., Wyrowski F., Yorke H. W., Yu S., Zmuidzinas J., Delorme Y., Desbat J.-P., Güsten R., Krieg J.-M., Delforge B. 1448 CH+(1-0) and 13CH+(1-0) absorption lines in Falgarone E., Godard B., Cernicharo J., de Luca M., Gerin M., Phillips T. G., Black J. H., Lis D. C., Bell T. A., A&A 521, L15 the direction of massive star-forming regions Boulanger F., Coutens A., Dartois E., Encrenaz P., Giesen T., Goicoechea J. R., Goldsmith P. F., Gupta H., Gry C., Hennebelle P., Herbst E., Hily-Blant P., Joblin C., Kaźmierczak M., KoŃos R., KreŃowski J., Martin-Pintado J., Monje R., Mookerjea B., Neufeld D. A., Perault M., Pearson J. C., Persson C., Plume R., Salez M., Schmidt M., Sonnentrucker P., Stutzki J., Teyssier D., Vastel C., Yu S., Menten K., Geballe T. R., Schlemmer S., Shipman R., Tielens A. G. G. M., Philipp S., Cros A., Zmuidzinas J., Samoska L. A., Klein K., Lorenzani A., Szczerba R., Péron I., Cais P., Gaufre P., Cros A., Ravera L., Morris P., Lord S., Planesas P. 1449 Herschel spectral surveys of star-forming Ceccarelli C., Bacmann A., Boogert A., Caux E., Dominik C., Lefloch B., Lis D., Schilke P., van der Tak F., A&A 521, L22 regions. Overview of the 555-636 GHz range Caselli P., Cernicharo J., Codella C., Comito C., Fuente A., Baudry A., Bell T., Benedettini M., Bergin E. A., Blake G. A., Bottinelli S., Cabrit S., Castets A., Coutens A., Crimier N., Demyk K., Encrenaz P., Falgarone E., Gerin M., Goldsmith P. F., Helmich F., Hennebelle P., Henning T., Herbst E., Hily-Blant P., Jacq T., Kahane C., Kama M., Klotz A., Langer W., Lord S., Lorenzani A., Maret S., Melnick G., Neufeld D., Nisini B., Pacheco S., Pagani L., Parise B., Pearson J., Phillips T., Salez M., Saraceno P., Schuster K., Tielens X., van der Wiel M. H. D., Vastel C., Viti S., Wakelam V., Walters A., Wyrowski F., Yorke H., Liseau R., Olberg M., Szczerba R., Benz A. O., Melchior M. 1450 Herschel observations in the ultracompact Fuente A., Berné O., Cernicharo J., Rizzo J. R., González-Garcìa M., Goicoechea J. R., Pilleri P., Ossenkopf A&A 521, L23 HII region Mon R2. Water in dense photon- V., Gerin M., Güsten R., Akyilmaz M., Benz A. O., Boulanger F., Bruderer S., Dedes C., France K., Garcìa- dominated regions (PDRs) Burillo S., Harris A., Joblin C., Klein T., Kramer C., Le Petit F., Lord S. D., Martin P. G., Martìn-Pintado J., Mookerjea B., Neufeld D. A., Okada Y., Pety J., Phillips T. G., Röllig M., Simon R., Stutzki J., van der Tak F., Teyssier D., Usero A., Yorke H., Schuster K., Melchior M., Lorenzani A., Szczerba R., Fich M., McCoey C., Pearson J., Dieleman P. 1451 The origin of the [C II] emission in the S140 Dedes C., Röllig M., Mookerjea B., Okada Y., Ossenkopf V., Bruderer S., Benz A. O., Melchior M., Kramer A&A 521, L24 photon-dominated regions. New insights C., Gerin M., Güsten R., Akyilmaz M., Berne O., Boulanger F., de Lange G., Dubbeldam L., France K., from HIFI Fuente A., Goicoechea J. R., Harris A., Huisman R., Jellema W., Joblin C., Klein T., Le Petit F., Lord S., Martin P., Martin-Pintado J., Neufeld D. A., Philipp S., Phillips T., Pilleri P., Rizzo J. R., Salez M., Schieder R., Simon R., Siebertz O., Stutzki J., van der Tak F., Teyssier D., Yorke H. 1452 Gas morphology and energetics at the Joblin C., Pilleri P., Montillaud J., Fuente A., Gerin M., Berné O., Ossenkopf V., Le Bourlot J., Teyssier D., A&A 521, L25 surface of PDRs: New insights with Herschel Goicoechea J. R., Le Petit F., Röllig M., Akyilmaz M., Benz A. O., Boulanger F., Bruderer S., Dedes C., observations of NGC 7023 France K., Güsten R., Harris A., Klein T., Kramer C., Lord S. D., Martin P. G., Martin-Pintado J., Mookerjea B., Okada Y., Phillips T. G., Rizzo J. R., Simon R., Stutzki J., van der Tak F., Yorke H. W., Steinmetz E., Jarchow C., Hartogh P., Honingh C. E., Siebertz O., Caux E., Colin B. 1453 The distribution of water in the high-mass Emprechtinger M., Lis D. C., Bell T., Phillips T. G., Schilke P., Comito C., Rolffs R., van der Tak F., Ceccarelli A&A 521, L28 star-forming region NGC 6334 I C., Aarts H., Bacmann A., Baudry A., Benedettini M., Bergin E. A., Blake G., Boogert A., Bottinelli S., Cabrit S., Caselli P., Castets A., Caux E., Cernicharo J., Codella C., Coutens A., Crimier N., Demyk K., Dominik C., Encrenaz P., Falgarone E., Fuente A., Gerin M., Goldsmith P., Helmich F., Hennebelle P., Henning T., Herbst E., Hily-Blant P., Jacq T., Kahane C., Kama M., Klotz A., Kooi J., Langer W., Lefloch B., Loose A., Lord S., Lorenzani A., Maret S., Melnick G., Neufeld D., Nisini B., Ossenkopf V., Pacheco S., Pagani L., Parise B., Pearson J., Risacher C., Salez M., Saraceno P., Schuster K., Stutzki J., Tielens X., van der Wiel M., Vastel C., Viti S., Wakelam V., Walters A., Wyrowski F., Yorke H. 1454 Water vapor toward starless cores: The Caselli P., Keto E., Pagani L., Aikawa Y., Yıldız U. A., van der Tak F. F. S., Tafalla M., Bergin E. A., Nisini A&A 521, L29 Herschel view B., Codella C., van Dishoeck E. F., Bachiller R., Baudry A., Benedettini M., Benz A. O., Bjerkeli P., Blake G. A., Bontemps S., Braine J., Bruderer S., Cernicharo J., Daniel F., di Giorgio A. M., Dominik C., Doty S. D., Encrenaz P., Fich M., Fuente A., Gaier T., Giannini T., Goicoechea J. R., de Graauw T., Helmich F., Herczeg G. J., Herpin F., Hogerheijde M. R., Jackson B., Jacq T., Javadi H., Johnstone D., Jørgensen J. K., Kester D., Kristensen L. E., Laauwen W., Larsson B., Lis D., Liseau R., Luinge W., Marseille M., McCoey C., Megej A., Melnick G., Neufeld D., Olberg M., Parise B., Pearson J. C., Plume R., Risacher C., Santiago- Garcìa J., Saraceno P., Shipman R., Siegel P., van Kempen T. A., Visser R., Wampfler S. F., Wyrowski F. 1455 Water in low-mass star-forming regions with Kristensen L. E., Visser R., van Dishoeck E. F., Yıldız U. A., Doty S. D., Herczeg G. J., Liu F.-C., Parise B., A&A 521, L30 Herschel. HIFI spectroscopy of NGC 1333 Jørgensen J. K., van Kempen T. A., Brinch C., Wampfler S. F., Bruderer S., Benz A. O., Hogerheijde M. R., Deul E., Bachiller R., Baudry A., Benedettini M., Bergin E. A., Bjerkeli P., Blake G. A., Bontemps S., Braine J., Caselli P., Cernicharo J., Codella C., Daniel F., de Graauw T., di Giorgio A. M., Dominik C., Encrenaz P., Fich M., Fuente A., Giannini T., Goicoechea J. R., Helmich F., Herpin F., Jacq T., Johnstone D., Kaufman M. J., Larsson B., Lis D., Liseau R., Marseille M., McCoey C., Melnick G., Neufeld D., Nisini B., Olberg M., Pearson J. C., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Shipman R., Tafalla M., Tielens A. G. G. M., van der Tak F., Wyrowski F., Beintema D., de Jonge A., Dieleman P., Ossenkopf V., Roelfsema P., Stutzki J., Whyborn N. 1456 Ortho-to-para ratio of interstellar heavy Vastel C., Ceccarelli C., Caux E., Coutens A., Cernicharo J., Bottinelli S., Demyk K., Faure A., Wiesenfeld A&A 521, L31 water L., Scribano Y., Bacmann A., Hily-Blant P., Maret S., Walters A., Bergin E. A., Blake G. A., Castets A., Crimier N., Dominik C., Encrenaz P., Gérin M., Hennebelle P., Kahane C., Klotz A., Melnick G., Pagani L., Parise B., Schilke P., Wakelam V., Baudry A., Bell T., Benedettini M., Boogert A., Cabrit S., Caselli P., Codella C., Comito C., Falgarone E., Fuente A., Goldsmith P. F., Helmich F., Henning T., Herbst E., Jacq T., Kama M., Langer W., Lefloch B., Lis D., Lord S., Lorenzani A., Neufeld D., Nisini B., Pacheco S., Pearson J., Phillips T., Salez M., Saraceno P., Schuster K., Tielens X., van der Tak F., van der Wiel M. H. D., Viti S., Wyrowski F., Yorke H., Cais P., Krieg J. M., Olberg M., Ravera L. Annual report 2010 57 1457 Water abundances in high-mass protostellar Marseille M. G., van der Tak F. F. S., Herpin F., Wyrowski F., Chavarrìa L., Pietropaoli B., Baudry A&A 521, L32 envelopes: Herschel observations with HIFI A., Bontemps S., Cernicharo J., Jacq T., Frieswijk W., Shipman R., van Dishoeck E. F., Bachiller R., Benedettini M., Benz A. O., Bergin E., Bjerkeli P., Blake G. A., Braine J., Bruderer S., Caselli P., Caux E., Codella C., Daniel F., Dieleman P., di Giorgio A. M., Dominik C., Doty S. D., Encrenaz P., Fich M., Fuente A., Gaier T., Giannini T., Goicoechea J. R., de Graauw T., Helmich F., Herczeg G. J., Hogerheijde M. R., Jackson B., Javadi H., Jellema W., Johnstone D., Jørgensen J. K., Kester D., Kristensen L. E., Larsson B., Laauwen W., Lis D., Liseau R., Luinge W., McCoey C., Megej A., Melnick G., Neufeld D., Nisini B., Olberg M., Parise B., Pearson J. C., Plume R., Risacher C., Roelfsema P., Santiago-Garcìa J., Saraceno P., Siegel P., Stutzki J., Tafalla M., van Kempen T. A., Visser R., Wampfler S. F., Yıldız U. A. 1458 Sensitive limits on the abundance of cold Bergin E. A., Hogerheijde M. R., Brinch C., Fogel J., Yıldız U. A., Kristensen L. E., van Dishoeck E. F., A&A 521, L33 water vapor in the DM Tauri protoplanetary Bell T. A., Blake G. A., Cernicharo J., Dominik C., Lis D., Melnick G., Neufeld D., Panić O., Pearson J. C., disk Bachiller R., Baudry A., Benedettini M., Benz A. O., Bjerkeli P., Bontemps S., Braine J., Bruderer S., Caselli P., Codella C., Daniel F., di Giorgio A. M., Doty S. D., Encrenaz P., Fich M., Fuente A., Giannini T., Goicoechea J. R., de Graauw T., Helmich F., Herczeg G. J., Herpin F., Jacq T., Johnstone D., Jørgensen J. K., Larsson B., Liseau R., Marseille M., McCoey C., Nisini B., Olberg M., Parise B., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Shipman R., Tafalla M., van Kempen T. A., Visser R., Wampfler S. F., Wyrowski F., van der Tak F., Jellema W., Tielens A. G. G. M., Hartogh P., Stützki J., Szczerba R. 1459 Hydrides in young stellar objects: Radiation Benz A. O., Bruderer S., van Dishoeck E. F., Stäuber P., Wampfler S. F., Melchior M., Dedes C., Wyrowski A&A 521, L35 tracers in a protostar-disk-outflow system F., Doty S. D., van der Tak F., Bächtold W., Csillaghy A., Megej A., Monstein C., Soldati M., Bachiller R., Baudry A., Benedettini M., Bergin E., Bjerkeli P., Blake G. A., Bontemps S., Braine J., Caselli P., Cernicharo J., Codella C., Daniel F., di Giorgio A. M., Dieleman P., Dominik C., Encrenaz P., Fich M., Fuente A., Giannini T., Goicoechea J. R., de Graauw T., Helmich F., Herczeg G. J., Herpin F., Hogerheijde M. R., Jacq T., Jellema W., Johnstone D., Jørgensen J. K., Kristensen L. E., Larsson B., Lis D., Liseau R., Marseille M., McCoey C., Melnick G., Neufeld D., Nisini B., Olberg M., Ossenkopf V., Parise B., Pearson J. C., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Schieder R., Shipman R., Stutzki J., Tafalla M., Tielens A. G. G. M., van Kempen T. A., Visser R., Yıldız U. A. 1460 Herschel observations of the hydroxyl radical Wampfler S. F., Herczeg G. J., Bruderer S., Benz A. O., van Dishoeck E. F., Kristensen L. E., Visser R., A&A 521, L36 (OH) in young stellar objects Doty S. D., Melchior M., van Kempen T. A., Yıldız U. A., Dedes C., Goicoechea J. R., Baudry A., Melnick G., Bachiller R., Benedettini M., Bergin E., Bjerkeli P., Blake G. A., Bontemps S., Braine J., Caselli P., Cernicharo J., Codella C., Daniel F., di Giorgio A. M., Dominik C., Encrenaz P., Fich M., Fuente A., Giannini T., de Graauw T., Helmich F., Herpin F., Hogerheijde M. R., Jacq T., Johnstone D., Jørgensen J. K., Larsson B., Lis D., Liseau R., Marseille M., McCoey C., Neufeld D., Nisini B., Olberg M., Parise B., Pearson J. C., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Shipman R., Tafalla M., van der Tak F. F. S., Wyrowski F., Roelfsema P., Jellema W., Dieleman P., Caux E., Stutzki J. 1461 Water in massive star-forming regions: HIFI Chavarrìa L., Herpin F., Jacq T., Braine J., Bontemps S., Baudry A., Marseille M., van der Tak F., A&A 521, L37 observations of W3 IRS5 Pietropaoli B., Wyrowski F., Shipman R., Frieswijk W., van Dishoeck E. F., Cernicharo J., Bachiller R., Benedettini M., Benz A. O., Bergin E., Bjerkeli P., Blake G. A., Bruderer S., Caselli P., Codella C., Daniel F., di Giorgio A. M., Dominik C., Doty S. D., Encrenaz P., Fich M., Fuente A., Giannini T., Goicoechea J. R., de Graauw T., Hartogh P., Helmich F., Herczeg G. J., Hogerheijde M. R., Johnstone D., Jørgensen J. K., Kristensen L. E., Larsson B., Lis D., Liseau R., McCoey C., Melnick G., Nisini B., Olberg M., Parise B., Pearson J. C., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Stutzki J., Szczerba R., Tafalla M., Tielens A., van Kempen T. A., Visser R., Wampfler S. F., Willem J., Yıldız U. A. 1462 The methanol lines and hot core of OMC2- Kama M., Dominik C., Maret S., van der Tak F., Caux E., Ceccarelli C., Fuente A., Crimier N., Lord S., A&A 521, L39 FIR4, an intermediate-mass protostar, with Bacmann A., Baudry A., Bell T., Benedettini M., Bergin E. A., Blake G. A., Boogert A., Bottinelli S., Herschel/HIFI Cabrit S., Caselli P., Castets A., Cernicharo J., Codella C., Comito C., Coutens A., Demyk K., Encrenaz P., Falgarone E., Gerin M., Goldsmith P. F., Helmich F., Hennebelle P., Henning T., Herbst E., Hily-Blant P., Jacq T., Kahane C., Klotz A., Langer W., Lefloch B., Lis D., Lorenzani A., Melnick G., Nisini B., Pacheco S., Pagani L., Parise B., Pearson J., Phillips T., Salez M., Saraceno P., Schilke P., Schuster K., Tielens X., van der Wiel M. H. D., Vastel C., Viti S., Wakelam V., Walters A., Wyrowski F., Yorke H., Cais P., Güsten R., Philipp S., Klein T., Helmich F. 1463 Herschel/HIFI observations of high-J CO lines Yıldız U. A., van Dishoeck E. F., Kristensen L. E., Visser R., Jørgensen J. K., Herczeg G. J., van Kempen A&A 521, L40 in the NGC 1333 low-mass star-forming T. A., Hogerheijde M. R., Doty S. D., Benz A. O., Bruderer S., Wampfler S. F., Deul E., Bachiller R., Baudry region A., Benedettini M., Bergin E., Bjerkeli P., Blake G. A., Bontemps S., Braine J., Caselli P., Cernicharo J., Codella C., Daniel F., di Giorgio A. M., Dominik C., Encrenaz P., Fich M., Fuente A., Giannini T., Goicoechea J. R., de Graauw T., Helmich F., Herpin F., Jacq T., Johnstone D., Larsson B., Lis D., Liseau R., Liu F.-C., Marseille M., McCoey C., Melnick G., Neufeld D., Nisini B., Olberg M., Parise B., Pearson J. C., Plume R., Risacher C., Santiago-Garcìa J., Saraceno P., Shipman R., Tafalla M., Tielens A. G. G. M., van der Tak F., Wyrowski F., Dieleman P., Jellema W., Ossenkopf V., Schieder R., Stutzki J. 1464 First detection of ND in the solar-mass Bacmann A., Caux E., Hily-Blant P., Parise B., Pagani L., Bottinelli S., Maret S., Vastel C., Ceccarelli A&A 521, L42 protostar IRAS16293-2422 C., Cernicharo J., Henning T., Castets A., Coutens A., Bergin E. A., Blake G. 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Alcolea OAN-IGN, Spain D. Muders, MPIfR, Germany Ph. André, CEA, France L. Tacconi (Chair), MPE, Germany Fr. Boulanger, IAS, France P. de Vicente, OAN-IGN, Spain P. Goldsmith, JPL, USA F. Wyrowksi, MPIfR, Germany S. Guilloteau (Vice-Chair), Obs. Bordeaux, France PROGRAM COMMITTEE H. Beuther, MPIA, Germany J.M. Girart, CSIC, Spain A. Blain, Caltech, USA M. Hogerheijde, Leiden, Netherlands S. Bontemps, Obs. de Bordeaux, France B. Lefloch, Obs. Grenoble, France P.-A. Duc, CEA, France E. Sturm, MPE, Germany J. M. Girart, CSIC, Spain A. Weiss, MPIfR, Germany A. Fuente, OAN-IGN, Spain C. Wilson, McMaster University, Canada S. Garcia-Burillo, OAN, Spain AUDIT COMMISSION C.N.R.S. B. Adans H. Redon M.P.G. M. Horstmann M. Mansfeld Millimétrique Institut de Radioastronomie IRAM IRAM Annual Report 2010 30-meter diameter telescope, Pico Veleta 6 x 15-meter interferometer, Plateau de Bure The Institut de Radioastronomie Millimétrique (IRAM) is a multi-national scientific institute covering all aspects of radio astronomy at millimeter wavelengths: the operation of two high-altitude observatories – a 30-meter diameter telescope on Pico Veleta in the Sierra Nevada (southern Spain), and an interferometer of six 15 meter diameter telescopes on the Plateau de Bure in the French Alps – the development of telescopes and instrumentation, radio astronomical observations and their interpretation. IRAM was founded in 1979 by two national research organizations: the CNRS and the Max-Planck-Gesellschaft – the Spanish Instituto Geográfico IRAM Addresses: Nacional, initially an associate member, became a full member in 1990. Institut de Radioastronomie The technical and scientific staff of IRAM develops instrumentation and Millimétrique 300 rue de la piscine, software for the specific needs of millimeter radioastronomy and for the Saint-Martin d’Hères benefit of the astronomical community. IRAM’s laboratories also supply F-38406 France Tel: +33 [0]4 76 82 49 00 devices to several European partners, including for the ALMA project. Fax: +33 [0]4 76 51 59 38 [email protected] www.iram.fr Front Cover IRAM’s scientists conduct forefront research in several domains of astrophysics, from nearby star-forming regions to objects at cosmological View of the Orion nebula, the closest Observatoire du Plateau de Bure distances. region of massive star forming Saint-Etienne-en-Dévoluy region, in the 12CO(2-1) emission, F-05250 France Tel: +33 [0]4 92 52 53 60 IRAM Partner Organizations: that traces the distribution of the Fax: +33 [0]4 92 52 53 61 Centre National de la Recherche Scientifique (CNRS) – Paris, France 2010 Annual Report cold (10-100 K) molecular gas. The Max-Planck-Gesellschaft (MPG) – München, Deutschland map was obtained using HERA at the Instituto de Radioastronomía Instituto Geografico Nacional (IGN) – Madrid, España 30-meter telescope and has spatial Milimétrica resolution of 12” (or 0.025 pc). The Avenida Divina Pastora 7, Local 20, E-18012 Granada, España dynamics of the molecular gas are Tel: +34 958 80 54 54 shown in blue (for the emission with Fax: +34 958 22 23 63 [email protected] velocities between –5 and 8 km/s) and in red (for velocities between Observatorio 12 and 25 km/s). The map in green Radioastronómico shows the emission from warm de Pico Veleta Sierra Nevada, (100 to 1000 K) dust and gas at the Granada, España surface of the clouds, traced at 8 Tel: +34 958 48 20 02 Fax: +34 958 48 11 49 microns by the Midcourse Space Experiment satellite. Designed and produced by rebusparis.com Printed in France (O. Berné et al. 2010)