iram infoNumber 74 February 2010

IRAM Grenoble300, rue de la Piscine, Domaine Universitaire, 38406, Saint Martin d’Hères, France Phone : +33 (0)4 76 82 49 00 Fax : +33 (0)4 76 51 99 38 email : info@iram.fr

The HERA CO-Line Extragalactic Survey (HERACLES) is a large program at the IRAM 30-m telescope that will reach completion in 2010. The goal of HERACLES is to obtain large area, sensitive maps of the distribution of molecular gas, as traced through the CO J=2 → 1 line, in a sizeable sample of (~45) nearby galaxies that cover a wide range of star formation rates, dynamical masses and Hubble types (first data are published in Leroy 2009, AJ, 137, 4670). These maps represent a key ingredient to study the distribution of interstellar gas in galaxies, how stars form out of this gas, and how conditions in different galaxies affect this process.

The enabling technology for HERACLES is the HERA array on the IRAM 30-m telescope. HERA, used in on-the-fly mapping mode allows the 30-m efficiently map CO emission across large areas of the sky, a capability clearly demonstrated by Schuster et al. 2007 (A&A, 461, 143) when they used HERA to map CO J=2 → 1 emission from the whole disk of M51. This allows complete inventories of molecular gas in significant samples of nearby galaxies, observations that were prohibitive with single-pixel receivers and interferometers. As a result HERACLES complements previous surveys of molecular gas in galaxies very well.

For example,the Five Colleges Radio Astronomy Observatory (FCRAO)Extragalactic CO Survey (Young 1995, ApJS, 98, 219), which remains the definitive survey of CO in the local volume, targeted hundreds of systems but only sampled the major axes of its targets. The BerkeleyIllinois Maryland Association Survey of Nearby Galaxies (BIMA SONG), the first systematic sample of large-area, high-resolution interferometer maps of CO emission

The HERA CO-Line Extragalactic Surveyby Adam K. Leroy and Fabian Walter on behalf of the HERACLES collaboration

Word from the Director

Dear IRAM Newsletter Readers,

You will find hereafter the latest issue of the IRAM Newsletter in a new edition. First, it will only be available electronically; second, we have designed a new layout that is in line with the recent IRAM web pages; third, we have rearranged its content giving a larger emphasis on technical developments, scientific results as well as interim reports on the large observing programs.

The IRAM Newsletter will appear twice per year around the time of the call of proposals, i.e. in February and July, providing useful information to the community before the deadline for the proposals’ submission.

Since the last issue of the IRAM Newsletter in September 2009, important events took place and new milestones were reached. Among them, the celebration of the 30 years of IRAM was a success and a report is given below.

On the technical side, the new correlator WIDEX, described in these pages, is now being commissioned on the Plateau de Bure and will soon become available to the community. This remarkable achievement opens up new observing possibilities including a significant sensitivity increase in the continuum as well as more spectral flexibility.

We hope that you will enjoy the new IRAM Newsletter.

Pierre Cox

continued on page 8

To the edges of the universe - 30 years of IRAMMore than 250 scientists, collaborators and official representatives joined the IRAM staff to celebrate the institute’s past, present and future.

Read more about the international conference on page 14.

2 IRAM Info N°74

Contents

Cover Story:The HERA CO-Line Extragalactic Survey

(by Adam Leroy and Fabian Walter) 1

Facilities: News from the PdB Interferometer 2

News from the 30m Telescope 3

Call for Proposals 4

Large Observing Programs 7

Director’s Discretionary Time 8

Scientific results:The HERA CO-Line Extragalactic Survey

(continued from page 1) 8

MAMBO-2 Science Highlights 10

Developments:WideX, the New PdBI Correlator 11

GISMO and NIKA at the 30m Telescope 12

News and Events:IRAM 30m Summerschool 2009 13

30 Years of IRAM 14

Meeting on HERA Data Processing 15

7th Interferometry School 2010 15

Observing with ALMA: Early Science 16

Staff Changes 16

Publications 17

Published by IRAM © 2010

Director Pierre Cox

Edited by Karin Zacher

Facilities

News from the Plateau de Bure Interferometerby Jan Martin Winters

This winter semester, the Plateau de Bure Interferometer already moved mid-December to the A configuration.

This most extended configuration will be kept until mid February, when it is planned to go to the B configuration.

continued on next page

Aluminum panels for antenna 2During last summers’ antenna maintenance period the reflector of antenna 2 was equipped with new aluminum panels, replacing the previous carbon fiber panels. The antenna was moved out of the maintenance hall on September 7 and the surface was subsequently adjusted to an accuracy of better than 50 µm rms in a series of holographic measurements and panel adjustments. Four out of the six Bure antennas are now equipped with an aluminum reflector, the remaining two antennas will follow during the summer 2010 maintenance period.

Installation of WideXAt the beginning of December 2009 the first unit of the new wide band correlator WideX (“Wideband Express’’) was installed on Plateau de Bure and first fringes were obtained by December 13 (see our NEWS section on the web). The remaining three units have been shipped to the Plateau beginning of February and the software integration and commissioning should be finished by end of February.

WideX will be able to simultaneously process two 3.6GHz wide IF bands (one per polarization). It will provide a fixed spectral resolution of 2MHz over the full 3.6GHz bandwidth and will be available in parallel to the existing narrow band correlator. All

information presently available on WideX can be found at http://www.iram.fr/IRAM-FR/TA/backend/WideX. We anticipate that WideX will become available for the second half of the current winter semester 2009/2010. Since the installation, testing, and commissioning of WideX has not yet finished at the time of writing this article, any observations requesting WideX can cur-rently be offered on a best effort basis only. We invite you to regularly check the NEWS section on our web page, where any progress in this matter will be posted.

Weather conditions and observ-ingThe current winter semester so far was affected by quite variable weather conditions with periods of excellent atmospheric stability and transparency in particular at the end of November and the beginning of January but with very poor weather during most of December. Bure entered into the winter observing period with the array in its C-configuration and we moved to the A configuration already on December 15. This most extended configuration will be kept until mid February, before going to the second most extended configuration B.

We currently anticipate to move back to the C configuration by beginning of March. The switch to the most compact D configu-ration is not foreseen before the beginning

http://www.iram-institute.org/EN/astronomers.php?ContentID=7&rub=7&srub=0&ssrub=0&sssrub=0http://www.iram.fr/IRAMFR/TA/backend/WideX/http://www.iram.fr/IRAMFR/TA/backend/WideX/http://www.iram-institute.org/EN/astronomers.php?ContentID=7&rub=7&srub=0&ssrub=0&sssrub=0

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News from the 30m Telescopeby Walter Brunswig, Albrecht Sievers and Carsten Kramer

TAPAS header data baseSince September 2009, all astronomical data headers from the IRAM 30m telescope are archived at the TAPAS header archive at IRAM/Granada, which is now online and accessible to the PIs of running projects. TAPAS is automatically and continuously filled with any new data. TAPAS provides a complete, homogeneous, and searchable database of the header information of all astronomical observations conducted at the 30m. It was built in a collaborative effort between IRAM and IAA/CSIC. And it contains more than 200 header variables for each observational scan, encompassing:· information on the observing setup (source, frequency, observing mode, etc.), ·information on the project (PI, Title, etc.), ·the status of the system at the time of the

observations (telescope, receiver, backend, weather, etc.), ·and also the results of calibrations, of pointing and focus scans. After a proprietary period of one year, a subset of the most important header data will be made publicly available at the Centre des Données astronomiques de Strasbourg (CDS).

We welcome and are keen to hear all users comments on the current database and suggestions on how it may be im-proved. Please contact tapasOperation@iram.es for technical questions.

The web link to TAPAS is given on the IRAM homepage, under science users, 30m telescope, Archive.

External USB disks 30m observers who expect to take more data than would fit on a few DVDs, i.e. more than about 10GB, are encouraged to bring an external USB disk to the 30m, to backup their data and take them home. The disk should be mountable under linux. Please contact the computer group (ncsOperation@iram.es) for technical information. Note that IRAM staff willcontinue to do a separate backup of all data, which is stored on the site.

of April. Global VLBI observations, which include the array in the 3mm phased-array mode, are planned from May 6 to 11, 2010. According to these plans, it will not be pos-sible to complete projects requesting deep integrations using the compact configura-tions before the end of the semester.

As far as A-rated projects are concerned,

we expect to bring most of these to comple-tion before the end of the current winter semester. B-rated projects are likely to be observed only if they fall in a favorable LST range. We remind users of the Plateau de Bure interferometer that B-rated proposals which are not started before the end of the winter semester have to be resubmitted.

Investigators, who wish to check the status of their project may consult the interferometer schedule on the Web athttp://www.iram.fr/IRAMFR/PDB/ongoing.html. This page is updated daily.

EMIR 330GHz bandThe E3 band has been successfully commissioned in November 2009, and is being heavily used in the ongoing winter semester 2009/10. For the two months October and November, at the end of the upcoming summer semester, we expect in total about a week of weather conditions better than 2mm of pwv, needed for E3 observations.

The E3 band employs sideband separation mixers for horizontal and vertical polarizations, and provides 4GHz of bandwidth per sideband. Sky frequencies between 260 and 350GHz can be tuned. Higher frequencies are at present not possible. At 340GHz, the telescope half

power beam width is 7.5’’. The aperture efficiency is 29% at this frequency, and at the optimum elevation of 49 degrees. The forward efficiency at this frequency is 81%. The 2mm and 0.9mm channels E150 and E330 are very well aligned: 0.75’’ ± 0.25’’. Pointing can be done at 2mm and then used for 0.9mm observations. The focus difference between E1 and E3 is ~ 250 µm. A detailed commissioning report is available online, on the EMIR home page.

mailto:tapasOperation@iram.esmailto:tapasOperation@iram.esmailto:ncsOperation@iram.eshttp://www.iram.fr/IRAMFR/PDB/ongoing.htmlhttp://www.iram.fr/IRAMFR/PDB/ongoing.html

4 IRAM Info N°74

The deadline for submission of observing proposals on IRAM telescopes, both the interferometer and the 30m, is

18 March 2010, 17:00 CET (UT+1h)

The scheduling period extends from 1 June - 30 November 2010. Proposals should be submitted through our web-based submission facility. Instructions can be found on our web page at URL:http://www.iram.fr/GENERAL/submission/submission.html

Detailed information on time estimates, special observing modes, technical information and references for both the IRAM interferometer and the IRAM 30m telescope can be found at this address:http://www.iram-institute.org/EN/ content-page

The submission facility will be opened about three weeks before the proposal deadline. Proposal form pages and the 30m

time estimator are available now.Please avoid last minute submissions

when the network could be congested. As an insurance against network congestion or failure, we still accept, in well justified cases, proposals submitted by:

fax to number: (+33) 476 42 54 69 or•ordinary mail addressed to: IRAM •Scientific Secretariat, 300, rue de la piscine, F-38406 St. Martin d’Hères, France

Proposals sent by e-mail are not accepted. Color plots will be printed/copied in grey scale. Proposals are evaluated on the basis of the paper copy. If color is considered essential for the understanding of a specific figure, a respective remark should be added in the figure caption. The color version may then be consulted in the electronic proposal by the referees.

Soon after the deadline the IRAM Scientific Secretariat sends an acknowledge-ment of receipt to the Principal Investigator of each proposal correctly received, together

with the proposal registration number. Note that the web facility allows cancellation and modification of proposals before the deadline. The facility also allows to view the proposal in its final form as it appears after re-compilation at IRAM. We urge propos-ers to make use of this feature as we always receive a number of corrupted proposals (figures missing, blank pages, etc.).

Valid proposals contain the official cover page, one or more pages of technical information, up to two pages of text describing the scientific aims, and up to two pages of figures, tables, and references. Normal proposals should not exceed 6 pages, except for additional technical pages. Longer proposals will be cut. We continue to call for Large Observing Programmes (see P. Cox in this Newsletter). The Large Programmes may have up to 4 pages for the scientific justification, plus cover page, the technical pages, and 2 pages for supporting material. Both proposal forms, for the 30m

Call for Proposals for the 30m Telescope and the Plateau de Bure InterferometerBy Clemens Thum and Jan Martin Winters

Covering the period from June to November 2010, this

year’s first proposal deadline for IRAM facilities will be

on March 18, 2010. As usual, the submission facility

will be opened about three weeks before the deadline.

Last year, more than 400 Proposals were received for

the IRAM 30m Telescope and the Plateau de Bure

Interferometer, testifying to an every increasing

interest of the scientific community in the institute’s

facilities.

Facilities

continued on next page

http://www.iram.fr/GENERAL/submission/submission.htmlhttp://www.iram.fr/GENERAL/submission/submission.htmlhttp://www.iram-institute.org/EN/content-page.php?ContentID=57&rub=7&srub=57http://www.iram-institute.org/EN/content-page.php?ContentID=57&rub=7&srub=57

February 2010 5

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telescope and for the interferometer, have been changed considerably. We now have different template files for the two telescopes, prop-pdb.tex and prop-30m.tex. Please, make sure to use the current version of these files and the common LATEX style file proposal.sty. All three files may be downloaded from:http://www.iram.fr/GENERALsubmission/proposal.html

Do not change the font type or size, and do not manipulate the style file. In case of problems, contact the IRAM secretary (e-mail: berjaud@iram.fr). Please, also indicate on the proposal cover page whether your proposal is (or is not) a resubmission of a previously rejected proposal or a continuation of a previously accepted interferometer or 30m proposal. We request that the proposers describe very briefly in the introductory paragraph (automatically generated header “Proposal history:”) why the proposal is being resubmitted (e.g. improved scientific justification) or is proposed to be continued (e.g. last observations suffered from bad weather).

Short spacing observations on the 30m telescope can be requested directly on the interferometer proposal form. A separate proposal for the 30m telescope is not required. The interferometer proposal form contains a bullet, labelled “short spacings’’ which should then be checked. The user will be prompted to fill in an additional paragraph in which the scientific need for the short spacings should be described. It is essential to give here all observational details, including size of map, sampling density and rms noise, spectral resolution, receiver configuration, and time requested.

A mailing list has been set up for astronomers interested in being notified about the availability of a new Call for Proposals. A link to this mailing list is on the IRAM web page. The list presently includes all principal investigators of proposals for IRAM telescopes during the last 2 years. Please verify that your email address in this list is correct.

Travel funds for European astronomersby Roberto Neri and Clemens Thum

Observations using IRAM telescopes continue to be supported by RadioNet under the European Framework Programme 7. A budget, somewhat reduced compared to the 2004 - 2008 period, is available for travel by European astronomers through the Trans National Access (TNA) Programme.

As before, travel may be supported to the 30m telescope for observation (contact: C. Thum) and to Grenoble for reduction of interferometer data (contact: R. Neri). Detailed information about the eligibility, policies, and travel claims can be found on the RadioNet home page. The Principal Investigators of IRAM proposals eligible for TNA funding will be informed individually.

Call for Observing Proposals on the 30m TelescopeBy Clemens Thum and Carsten Kramer

SummaryProposals for three types of receivers will be considered for the coming summer semester (1 June - 30 November 2010): 1. the heterodyne receiver EMIR, consisting of dual-polarization mixers,

operating in the four bands at 3, 2, 1.3, and 0.9mm wavelengths. 2. the 9 pixel dual-polarization heterodyne receiver array, HERA, operating at 1.3mm wavelength. 3. the MAMBO2 bolometer array with 117pixels operating at 1.2mm.

About 2000 hours of observing time are expected to be available. During the months May to September, emphasis will be put on observations at the longer wavelengths. During October and Novem-ber, we will schedule observing pools for MAMBO2, HERA, poor weather backup projects, and projects which need very good weather conditions of better than 2mm of precipitable water vapor (pwv). We con-tinue to call for Large Programmes using any of the three instruments.

What is new?Observation time estimatorWe now offer a new web based time estimator for all three instruments, EMIR, HERA, and MAMBO2. The web interface is available via the 30m homepage. Proposers are requested to use these new time estimators.

Proposal formMotivated by the requirement for weather based scheduling, the proposal form for the 30m telescope has been modified. The tables on the Technical Summary page now stipulate for input of the amount of precipitable water vaper acceptable for the proposed observation.

continued on next page

http://www.iram.fr/GENERAL/submission/proposal.htmlhttp://www.iram.fr/GENERAL/submission/proposal.htmlhttp://www.iram.fr/mailman/listinfohttp://www.radionet-eu.org

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Technical issuesApart from ongoing work to improve the telescope control software (NCS), we expect to spend about 2 weeks of telescope time on further tests of the transition edge (TES) and KID bolometer arrays GISMO and NIKA. Both instruments currently work at 2mm.

Some gear boxes of the telescope main axes drives have recently shown signs that they are approaching the end of their useful lives. We plan to replace the two units with the most damage during summer. This is a complicated manoevre, the first of this kind during the 25 years of telescope operation and not without some risk. Over the coming years, we plan to eventually replace or repair all gear boxes.

Work is ongoing to implement the new Fourier Transform Spectrometers (FTS), with the goal to start making them available in the coming winter semester.

The complete textof the Call for Proposals, including a detailed description of EMIR capabilities, can be retrieved as a pdf file from the IRAM web site at http://www.iram.fr/GENERAL/ calls/s10/s10.pdf.

Call for Observing Proposals on the Plateau de Bure Interferometerby Jan Martin Winters

Conditions for the next summer periodAs every year, we plan to carry out extensive technical work during the summer semester, including the regular maintenance of the antennas. In particular, the last two antennas will be fully equipped with new aluminum panels replacing their current carbon fiber panels. Additionally it is foreseen to install a new LO system on Plateau de Bure that will considerably reduce the instrumental phase noise, particularly important for observations at high frequencies. This upgrade implies that observations with the interferometer will have to be stopped for about one week. Installation of the new band 4 mixers (covering the 350GHz atmospheric window) in the remaining four antennas is planned in parallel with the antenna maintenance and should not cause any further downtime of the interferometer. Testing of the new system and in particular of the 350GHz mixers will however require some excellent observing conditions toward

the end of the upcoming scheduling period.During the maintenance period, regular

scientific observations will mostly be carried out with the five element array. We plan to start the maintenance at the latest by the end of May and to schedule the 5D con-figuration between June and October.

We strongly encourage observers to submit proposals that can be executed dur-ing summer operating conditions. To keep the procedure as simple as possible, we ask to focus on:

observations requesting the use of the •2mm and 3mm receiverscircumpolar sources or sources •transit ing at night between June and September,observations that qualify for the 5D, •6D, and 6C configurations

Part of the projects will be scheduled at the end of the summer period when the six-element array (likely in C-configuration) is expected to be back to operation. Projects that should be observed with a subset of the

During the summer semester, a new LO system will be installed on the Plateau de Bure that will considerably reduce the instrumental phase noise, particularly important for observations at high frequencies

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Assembly of the GISMO bolometer: optical system, fridge and squids amplifier box.

Additionnal tests of the transition edge (TES) and KID bolometer arrays GISMO and NIKA are scheduled at the Pico Veleta Telescope during this winter semester.

http://www.iram.fr/GENERAL/calls/s10/s10.pdfhttp://www.iram.fr/GENERAL/calls/s10/s10.pdf

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five-element array will be adjusted in uv-coverage and observing time.

ReceiversAll antennas are equipped with dual polarization receivers for the 3mm, 2mm, and 1.3mm atmospheric windows. The frequency range is 80GHz to 116GHz for the 3mm band, 129GHz to 174GHz for the 2mm band, and 201 to 267GHz for the 1.3mm band.

Local ContactA local contact will be assigned to every A or B rated proposal which does not involve an in-house collaborator. He/she will assist you in the preparation of the observing procedures and provide help to reduce the data.

Assistance (write to sog@iram.fr) is also provided before a deadline to help new-comers in the preparation of a proposal.

Depending upon the program complexity, IRAM may require an in-house collaborator instead of the normal local contact.

Technical pre-screeningAll proposals will be reviewed for technical feasibility in parallel to being sent to the members of the program committee. Please help in this task by submitting technically precise proposals. Note that your proposal must be complete and exact: the source position and velocity, as well as the requested frequency setup must be correctly given.

DocumentationThe documentation for the IRAM Plateau de Bure Interferometer includes documents of general interest to potential users and more specialized documents intended for observers on the site (IRAM on-duty astronomers, operators, or observers with

non-standard programs). All documents can be retrieved on the Internet at http://www.iram.fr/IRAMFR/PDB/docu.html.

The complete text of the Call for Pro-posals can be retrieved from the IRAM web site at http://www.iram.fr/GENERAL/calls/s10/s10.pdf.

Quality of ProposalsFinally, we would like to stress again the importance of the quality of the observing proposal.

The IRAM interferometer is a powerful, but complex instrument, and proposal preparation requires special care. Information is available in the call for proposals and at http://www.iram.fr/IRAMFR/PDB/docu.html. The IRAM staff can help in case of doubts if contacted well before the deadline.

Note that the proposal should not only justify the scientific interest, but also the need for the Plateau de Bure Interferometer.

Facilities

Large Observing Programsby IRAM Director Pierre Cox

IRAM offers the possibility to apply for observing time in the framework of a Large Program for the 30-meter telescope and the Plateau de Bure interferometer.

A Large Program should require a minimum of 100 hours of observing time, spread over a maximum of two years, i.e. 4 contiguous semesters. IRAM will accept a limited number of Large Programs to be carried out per semester and instrument (30-meter and Plateau de Bure interfero-meter), allocating a maximum of 30% of observing time to such projects.

The Large Program should address strategic scientific issues leading to a break-through in the field. Large Programs should be coherent science projects, not reproduc-ible by a combination of smaller normal proposals.

The Large Program proposals should contain a solid management plan ensur-ing an efficient turnover, including data reduction, analysis, and organization of the efforts.

Because of the large investment in

observing time, but also of the inherent support from IRAM, it is advised that Large Programs involve one or more IRAM inter-nal collaborators.

During the execution period of the Large Programs (ideally before mid-term), the team leading the Large Program should report to IRAM about the preliminary results and possible technical difficulties, so that IRAM could assess the progress made, assist with any problems encountered in the course of the observations, and, if needed, adjust the program scheduling.

The proprietary period ends 18 months after the end of the last scheduling semester in which the Large Program was observed. The raw data and processed data then enter the public domain. An extension of this proprietary period may be granted in excep-tional cases only. A corresponding request will have to be submitted to the IRAM director.

Because of the scope of the Large Pro-grams and the need to explain the organiza-tion of the project, Large Program proposals

Galaxy NGC 4736 observed with the IRAM 30m Telescope. The galaxy is part of HERACLES (HERA CO-Line Extragalactic Survey), a Large Program that will reach completion in 2010 (see page 1).

IRAM offers the possibility to apply for observing time in the framework of a Large Program for the 30m Telescope and the Plateau de Bure Interferometer, which enables astronomers to cover strategic scientific issues leading to a breakthrough in the field.

continued on next page

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will have a maximum length of 4 pages (not including figures, tables, or references), instead of the 2 pages for normal proposals. Large observing program proposals should be submitted using the standard proposal templates; just check the “Large Program’’ bullet on the cover page. The following sections should be included: i) Scientific Rationale, ii) Immediate Objective, iii) Fea-sibility and Technical Justification, and iv) Organizational Issues. For the Plateau de Bure interferometer, the latter section must include a consideration of sun avoidance

constraints and configuration scheduling.The scientific evaluation of the Large

Program proposals will be done by the Pro-gram Committee at large (all 12 members, except if there is a direct implication of one of the members in the proposal). External reviewers will be asked to evaluate Large Programs, if needed. In addition to the scientific evaluation, there will be an assess-ment of the technical feasibility by IRAM staff.

Note that a Large Program will either be accepted in its entirety or rejected, there

will be no B-rating (“backup status’’) nor a partial acceptance/rejection of the proposal.

For the summer semester 2010, the call for Large Programs will be open for the 30m telescope and the Plateau de Bure interferometer. For the 30m telescope, Large Programs may consider using HERA and MAMBO, as well as EMIR. Observa-tions on the Plateau de Bure that are re-questing WideX are offered on a best effort basis for the upcoming summer semester 2010.

Director’s Discretionary Time Proposalsby Pierre Cox

Which proposals qualify for a DDT request?A small fraction of the available observing time at the Plateau de Bure interferometer and the 30-meter telescope can be assigned to Director’s Discretionary Time Proposals (DDT).

A DDT proposal must fulfill at least one of the following criteria:

* Proposals of Target-of-Opportunity (ToO) nature requiring the immediate ob-servation of an unanticipated, short-lived astronomical event;

* Proposals that are urgent either addressing highly competitive scientific topics or asking for observations that will lead to break-through results or requesting follow-up observations of recent discover-ies using ground or space facilities that re-quire urgent complementary IRAM data.

* Proposals testing news ideas or including an element of risk, that can be tested with small amounts of observing time

How to submit a DDT ProposalDDT proposals may be submitted any time. They must be written using the regular 30-meter or Plateau de Bure interferometer proposal template and should be sent to the IRAM Director (ddt@iram.fr) in attachment to an e-mail (tex files AND postscript files), specifying

in the subject field of the e-mail: DDT Proposal for the 30-meter telescope / Plateau de Bure interferometer.

DDT proposals should include a clear justification why the program should be considered for DDT allocation and was not submitted for the regular proposal deadline.

Please indicate on the proposal cover page if the proposed DDT observations are related to a previous or an on-going IRAM program. If so, the corresponding proposal number should be indicated.

Proposal evaluationDDT proposals will be evaluated in swift manner, in particular the ToO proposals. For other DDT proposals provide a minimum of two weeks notice for the time requested.

Please note that within one month following the observations, the PI of an accepted DDT proposal should submit a feedback report to the IRAM Director (ddt@iram.fr).

Scientific Resultscontinued from page 1

from galaxies covers a relatively smaller area than HERACLES with somewhat lower sensitivity in each system but with higher resolution (~6” compared to ~13”).Overlap with heterodyne-array based surveys of other CO transitions in nearby galaxies by Wilson et al. 2009 (ApJ, 693, 1736) and Kuno et al. 2007 (PASJ, 59, 117) also allows measurements of the excitation of molecular gas in different environments.

The other key characteristic of HERACLES is the sample, which is among the best-studied in the local universe. HERACLES was designed share the targets of The HI Nearby Galaxy Survey (THINGS, Walter et al. 2008, AJ, 136, 2563) and the Spitzer Infrared Nearby Galaxies Survey (SINGS, Kennicutt et al. 2003, PASP, 115, 928), ensuring an immediately accessible multi-wavelengthdatabase spanning from radio to UV. These data offer windows on the diffuse ISM, dust, embedded star formation, photodissociation regions, and both young and old stars. Because these targets are relatively close, the ~13” angular resolution of HERA translates to ~500pc at the median distance of our sample; as a result, all of these important physical quantities are known at many positions across each galaxy.

Figure 1 (see next page) shows a subset of the HERACLES targets. As discussed in Leroy et al. (2009, AJ, 137, 4670), although the channel and integrated intensity

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http://www.iram.fr/GENERAL/submission/proposal.htmlmailto:ddt@iram.fr

February 2010 9

maps show a variety of morphologies, the azimuthally averaged profiles are well-described by exponential declines. The best-fit scale lengths range from 0.8-3.2kpc and correlate closely with optical radius, near-IR (stellar mass) scalelength, and UV+IR (star formation) scale length. These results are in goodagreement with previous findings that CO emission closely follows both thestellar light and distribution of star formation on large scales. Thee xponential decline in CO brightness is a combination of decreasing maximum brightness of CO emission and a decreased filling fraction of bright CO emission at large radii.

To date, two papers have been published that present the first roundof in-depth scientific analysis. InBigiel et al. 2008 (AJ, 136, 2846) we combined HERACLES with HI, IR and UV data to measure the relationship between the surface densities of HI, H2, and star formation rate (the ‘star formation law’, Figure 2). In Leroy et al. 2008 (AJ, 136, 2782) we used the same data to measure the star formation per unit gas as a function of environment, comparing these measurements to proposed theories. There are currently a number of ongoing science projects within the

HERACLES collaboration, including an extended analysis of the star formation law, a comparison of the HI and H2 kinematics (including using the CO emission to accurately sample the inner parts of the rotation curves where HI is faint), and a comparison of arm and inter-arm gas and star formation. Other projects underway include a study of the gas excitation, the dense molecular gas phase, and a study of the gas-to-dust ratio (with a derivation of possible constraints on the CO-to-H2

conversion factor) of the HERACLES sample.

A HERACLES team meeting with the first presentations on the various science projects will be held at the MPIA Heidelberg at the end of February 2010. A public data release of HERACLES is planned one year after the data taking is completed (observations are projected to be completed, weather permitting, by Summer of 2010).

Results

The HERACLES team is an international

collaboration lead by Adam Leroy (NRAO)

and Fabian Walter (MPIA). The HERACLES

team members are: Frank Bigiel (UC

Berkeley), Elias Brinks (Herfordshire),

Daniela Calzetti (UMass), W.J. G. de Blok

(Cape Town), Gaelle Dumas (MPIA),

Kelly Foyle (MPIA), Robert C. Kennicutt

(Cambridge), Carsten Kramer (IRAM),

Sharon Meidt (MPIA), Hans-Walter Rix

(MPIA), Eric Rosolowsky (UBC), Helene

Roussel (IAP), Karin Sandstrom (MPIA),

Eva Schinnerer (MPIA), Andreas Schruba

(MPIA), Karl Schuster (IRAM), Antonio

Usero (OAN Madrid), Helmut Wiesemeyer

(IRAM) and Axel Weiss (MPIfR).

Fig. 1: CO (2-1) emission in nearby galaxies observed using HERA.

Fig.2: The star formation law (star formation surface density as a function of gas surface density) based on the HERACLES and THINGS datasets (colored contours). A complex behavior is seen that is due to different physical regimes in which star formation is occurring. For details see Bigiel et al. 2008 (AJ, 136, 2846).

10 IRAM Info N°74

Results

Here, we will present a few highlights of the MAMBO-2 pooled weeks of the summer semester 2009, which had been scheduled in November 2009.

After a test run of the NIKA bolometer and re-installation by the Granada receiver group, MAMBO-2 was recommissioned by Guillermo Quintana-Lacaci, with help by Robert W. Zylka and Albrecht Sievers.

A total of 216 hours were allocated for the following pool. The observations of this pool period, in general, enjoyed good to excellent weather conditions reaching below 1mm of water vapor. About 40 hours were used for HERA observations, as the wobbler could not be used during this period, 64 hours were used for heterodyne backup projects, and about 2 days were lost due to bad weather.

The figures show two science highlights of this pool session. Román-Zuñiga et al. obtained a map of the central region of Barnard 59 and Frieswijk et al. obtained a map of the cold dust emission of proto-clusters in the cluster-forming clump G111.

MAMBO2 - Science Highlights November 2009by Guillermo Quintana-Lacaci and Carsten Kramer

Fig.1: 1.2 mm continuum emission of the central region of Barnard 59 obtained with MAMBO-2 (Román-Zuñiga et al.).

Fig. 2: The 1.2 mm MAMBO-2 map of the continuum emission in the G111 cluster (Frieswijk et al.).

February 2010 11

Developments

The New WideX Correlatorby Marc Torres

Fully deliveredEarly December 2009, the first quarter of Widex was made available to PdB and connected to the existing receivers and computers. After a short period, fringes of excellent quality were obtained at 3mm, validating the real-time delay and phase tracking.

The 4 units were supposed to be built at the same time, but a loss in quality at the subcontractor level has requested re-work on many modules, causing a 6 week delay. Eventually the system could be completed and thoroughly tested in the Grenoble labs. In the meantime, all WideX units have been shipped to the Plateau de Bure and are now installed in the correlator room. The software integration and commissioning of the instrument should be finished by end of February.

WideX allows 4 GHz of frequency coverage on two simultaneous polarizations. It can be operated together with the existing correlator, which is now better used for narrowband work.

For more information:http://www.iram.fr/IRAMFR/TA/backend/WideX or just type “widex correlator backend” in your favorite search engine!

WideX Chronology

02/2007 Decision to extend WideX to 8 antennas and 2 MHz resolution.

06/2007 ASIC design kickoff

11/2007 Computer interface & test software design

02/2008 Backplane defined

07/2008 Prototype correlator card test

09/2008 FPGA code beta version

03/2009 First half unit (WideX 0.5) functional

09/2009 Fully equipped 1st unit, thermal tuning

02/2010 All 4 units installed on site

On December 13, 2009 IRAM astronomers got first astronomical light with the WideX first unit.

They were able to observe stable fringes towards the quasar 3C454.3 and the narrow band

correlator on all fifteen baselines of the Plateau de Bure interferometer.

The figure shows the Orion spectrum around 87 GHz measured with the old correlator and

WideX.

http://www.iram.fr/IRAMFR/TA/backend/WideXhttp://www.iram.fr/IRAMFR/TA/backend/WideX

12 IRAM Info N°74

Developments

Early 2007 a call for letter of interest was issued by IRAM with the goal to replace the 117 pixels MAMBO-2 bolometer array (which is based on semi-conductor technology) by a new instrument with an increased sensitivity, a wider field of view, with more pixels, possibly arranged in a filled array, and eventually able to observe in two frequency bands. The significant improvements announced in the specifications are based on the fundamental limits of the angular resolution of the 30m Telescope, its future increased field of view, and the background photon noise under good weather conditions (which gives NET ~ 1 mK· √s and NEFD ~ 10 mJy· √s in source tracking mode).

Two prototype cameras based upon different technologies and built by different groups have been successfully tested at Pico Veleta. Both work in the 2mm band, whereas MAMBO-2 operates at 1mm. The major differences of these prototypes compared to MAMBO-2 are the absence of feedhorns and the detectors’ technology. The absence of feedhorns will enable to know whether it is possible to achieve good detection efficiencies and good stray light rejections with bare pixels so that, when arranged in filled arrays, they not only cover the complete field of view without holes, but also increase the robustness against the spatial component of the anomalous refraction from the atmosphere (that can be responsible for signal losses while observing point sources with feedhorns).

The first prototype tested was GISMO (Goddard IRAM Superconducting 2-Millimeter Observer), built by a team lead by Johannes Staguhn from the Goddard Space Flight Center. The detector part of the instrument is an array of 8x16 multiplexed Transition Edge Sensor bolometers (the electric resistance of a TES thermometer cooled at the normal-superconducting transition increases with

the heat created by incoming photons). The multiplexing is realized in the time domain thanks to SQUID switches.

Two test runs were performed at Pico Veleta in November 2007 and October 2008. Besides some youth problems such as significant portions of unusable pixels, and immature detector control and data reduc-tion, the runs were encouraging for several reasons: quick instrument installation and alignment, convenient real time display and quick look analysis, easily fixable problems to get a good pixels yield, and above all, an apparently reachable background limited sensitivity.

The second prototype tested was NIKA, the Néel IRAM KIDs Array, built by Alain Benoit’s group from the Institut Néel in collaboration with other groups from SRON, AIG Cardiff and IRAM. Its cryostat can accommodate various detector technologies, but at the end of 2008, when the collaboration was formed (joining the complementary work done so far by each group), it was decided to put most of the receiver efforts into the development of Kinetic Inductance Detectors (the complex impedance of a resonant micro-strip coupled to an absorbing antenna, both forming the KID, is shifted relatively to the energy deposited by the incoming photons). This technology is fairly recent, but progressed rapidly during the last few years. Thanks to a small number of microfabrication steps, KIDs are easier to fabricate than concurrent technologies. They also offer intrinsic possibilities for multiplexing a great number of detectors in the frequency domain on a single readout line. However, beside numerous developments around the world no KID had shown satisfactory performances on a telescope so far. In this regard the test run of NIKA at the 30m telescope in November 2009 was a successful première, since various astronomical objects were observed with the two different types of KID arrays

GISMO and NIKA at the 30m Telescopeby Samuel Leclercq

GISMO (Godard IRAM Superconducting 2-Millimeter Observer), a 8x16 array (shown here in its detector package) is equipped with Transition Edge Sensors. This technology is based on the modification of a resitance on the normal-superconducting transition due to a local heating by the incoming photons.

GISMO performed two promising test runs at the 30m Telescope in 2007 and 2008.

NIKA (Néel IRAM KIDs Array), a 6x7 array (shown mounted on its cryostat) is equipped with Kinetic Inductance Detectors. This technology is based on the modification of the resonant characteristics of a superconducting micro-structure sensitive to the incoming photons.

NIKA performed a run at the 30m Telescope in 2009, which was encouraging for both arrays tested (a 6x7 antenna KID array with micro-lenses, and a 5x6 Lumped Element KID array).

continued on next page

February 2010 13

Developments

tested: a 6x7 antenna coupled KID built by SRON, and a 5x6 Lumped Element KID developed by Néel, IRAM and AIG Cardiff. For both arrays the sensitivities are still between 1 and 2 orders of magnitude away from the background limits, but work to improve the instrument is in progress.

The runs of GISMO and NIKA have been important steps in the framework of the bolometer replacement project for the 30m Telescope. They not only served as live tests of the detector technology (in particular for NIKA) and sensitivity (in particular for GISMO), but also allowed us to learn interfacing these new instruments with the telescope. Improved versions of GISMO and NIKA will be tested again in the course of 2010.

Cassiopeia A seen by GISMO in the 2 mm continuum emission. Cas A is a supernova remnant in the constellation Cassiopeia and the brightest astronomical radio source in the sky.

News and Events

IRAM 30m Summerschool 2009by Carsten Kramer

The 5th 30m Summerschool 2009 “Paving the way: From Millimeter to Far-Infrared Astronomy”, was held in the week of September 4 to 14. Like the previous schools, it was held in the ski resort Pradollano, in the Sierra Nevada, at only 15 minutes driving distance from the 30m telescope. The school was attended by 42 students from all over Europe, and from Chile, USA, India, and China.

Lectures and about 40 hours of observing time were spent, to cover the main topics of this school: “Galactic Nuclei” led by S.Garcia-Burillo and R.Aladro, “Millimeter observing techniques: calibration and imaging of spectral line data” by B.Lefloch

and A.Sievers, “Photon dominated regions” by J.Pety, S.Bardeau, and B.Ocana, “Magnetic fields and polarimetry” by C.Thum and D.Riquelme, “Mapping of nearby galaxies” by A.Leroy and C.Buchbender, “Bolometers and dust emission in the universe” by A.Weiss and G.Quintana-Lacaci. Additional lectures on the “Solar System” by R.Moreno and “Millimeter astronomy linked to the far-infrared” by C.Kramer, further broadened the scope of the school.

One highlight of the school, was the lecture of E.Caux on the science capabilities and present status of the Herschel Space Observatory and its three instruments.

Another highlight was the visit of the Albayzin and the Alhambra in Granada. All lectures and group presentations are available online via the IRAM homepage. This school was partially funded by the RadioNet FP7 program.

The 2 mm continuum emission of Messier 87 seen by NIKA. M87 is a giant elliptical galaxy, containing an active nucleus.

Both images were obtained in only a few minutes of integration, illustrating the potential of GISMO and NIKA. Several brighter and fainter sources were also observed during the test runs of both instruments.

14 IRAM Info N°74

News and Events

To the Edge of the Universe: 30 Years of IRAM – An International Conferenceby Pierre Cox and Karin Zacher

The year 2009 marked the 30th anniversary of the creation of IRAM. The institute was founded in 1979 by the French CNRS (Centre National de la Recherche Scientifique), the German MPG (Max-Planck-Gesellschaft) and the Spanish IGN (Instituto Geográfico Nacional), initially an associate member, becoming a full member in 1990. The story of IRAM represents a trailblazing European scientific and technical partnership that has set new standards in millimeter radio astronomy.

Over the last 30 years, the IRAM telescopes have been at the origin of a large number of spectacular discoveries. The goal of the conference was to review the main results obtained with the IRAM telescopes, from cosmology to the solar system, and to present the technical developments that enabled these observations. The conference also discussed the impact of these advances on millimeter and sub-millimeter astronomy and outlined future plans for upgrading the IRAM telescopes. The celebration of IRAM’s 30 years was an opportunity to examine new scientific

horizons that will be opened by the next generation of radio telescopes, and to explore the role that IRAM will continue to play in the rapidly evolving landscape of radio-astronomy.

The conference that took place in Grenoble on September 28th – 30th, 2009 was very successful, attracting more than 250 participants, including scientists, official representatives and past and present IRAM collaborators. All the presentations were of a high quality, providing a vivid picture of the scientific output based on the IRAM facilities. Many of those who took part in the beginnings of IRAM were also present and gave overviews about the creation of the institute and its first years that lead to the success of today. The future of IRAM was also discussed and there was a strong support for the Northern Extended Millimeter Array (NOEMA) project, a major upgrade of the Plateau de Bure interferometer.

As this conference was also a celebration, social events enlightened these three days with an unforgettable ‘birthday party’ on the first evening and, on the second day, a dinner at the Chateau du Touvet, where a speech in honor of Michael Grewing, the

former IRAM director, was given. The conference was a clear highlight of the year 2009 and a milestone in the history of IRAM bringing together four generations of astronomers and engineers without whom IRAM would not have been possible. Unfortunately, one of the founders of IRAM, Emile-Jacques Blum, passed away a few days before the conference started. The conference was dedicated to his memory.

In one of his last messages, responding to our invitation to give a speech, Emile-Jacques Blum finished with a sentence by which we would also like to conclude this short summary:

‘Succès et longue vie à l’IRAM !!’.

The year 2009 was not only the International Year of Astronomy but also IRAM’s 30th anniversary. The international conference that celebrated this event was clearly one of the institute’s highlights of last year.

The “38 Tonnes”, one of Grenoble’s most distinguished brass bands, started the evening program and transformed IRAM’s birthday cocktail into a most enjoyable party.

February 2010 15

News and Events

Meeting on HERA Data Processingby Karl Schuster, IRAM Deputy Director

With the number of relatively large data sets from HERA steadily increasing over time, the necessity for specific user exchange and for discussion of topics related to instrumental details, observing strategy, data reduction and interpretation has been recognized. IRAM has therefore organized a dedicated working meeting. The meeting took place the 9th and 10th of December in Grenoble.

The goals of the meeting were to:report on HERA status and generate •input for improvements, calibration and control software.exchange on observational strategies •and their effect on data quality.discuss optimum reduction of existing •datareport on plans for future multibeam •instruments and receive feedback on specific technical choices such as derotation and pixel arrangements.report status and ongoing development •in GILDAS which are relevant for Multibeam data.

K. Schuster reported on the technical status of HERA with focus on detailed pixel positions, current noise & stability

performance, image gain as well as derotator control. As some users reported offsets as compared to nominal a re-characterization campaign will be planned. The usefulness of prepared flat-fielding procedures was emphasized by the participants. An improvement of the derotator control during pointing was recognized as necessary.

H. Ungerechts reported on the current status of PAKO/NCS and proposed to extend scanning modes to more complex curves. H. Wiesemeyer reported on HERA pooling and the MIRA developments including new features for calibration using the initial and final part linear scans. J. Petit reported on the status of GILDAS and developments relevant for multibeam data within.

P. Hily-Blant reported on galactic large scale mapping using FSW and related flat-fielding based on a statistical approach using the sums of signals for each pixels and subsequent equalizing. N. Marcelino reported on the Orion mapping project and discussed possible problems with pixel offsets. F. Wyrowski reported mapping with the CHAMP+ receiver at APEX. Q. Nguyen presented the preliminary

results of a large mapping project in the galactic plane (W43).

On extragalactic mapping A. Leroy described observational strategy and data reduction for the HERACLES nearby galaxy project using basket weaving and HI defined baseline windows. J. Braine reported on the M33 CO(2-1) mapping project, gridding strategies and cloud extraction.

A round table discussion was held towards the end of the meeting to discuss new possible observing modes such as WSW OTF, the status of the telescope and possible error beam deconvolution. A great number of very useful general comments and suggestions from HERA users could be collected during this meeting. It is planned to use this way of organizing specific working meetings to cover other topics in the future.

Participants:

J. Braine (Obs Bordeaux), P. Carloff (KOSMA), P. Hily-Blant (LAOG), A. Leroy (NRAO), N. Marcelino, Q.Nguyen-Luong (CEA Saclay), P. Schilke (KOSMA), F. Wyrowski (MPIfR), and from IRAM: M. Gonzalez, A.L. Fontana, C. Kramer, D. Maier, J. Pety, N. Rodriguez, H. Ungerechts, K. Schuster, H. Wiesemeyer.

7th IRAM Millimeter Interferometry School 4th - 8th Oct. 2010by Frédéric Gueth

IRAM will organize this year its 7th millimeter-interferometry school. These schools are organized every two years since 1998. The 7th school will take place at the IRAM headquarters (Grenoble, France) on October 4 - 8th, 2010. It is intended for PhD students, post-docs and scientists who want to acquire a good knowledge of interferometry and data reduction techniques at millimeter wavelengths. The program will include lectures on:- Fundamentals of millimeter interferometry

- Atmospheric phase correction- Data calibration and imaging techniques- The IRAM Plateau de Bure interferometer- The Atacama Large Submillimeter/Millimeter Array (ALMA)

Tutorials will also be organized to help participants to become familiar with the reduction of Plateau de Bure data.

This event is supported by RadioNet and is part of the activities of the IRAM node of the European ALMA Regional Center (ARC). Registration is free of charge

but the school can accept only up to 60 par-ticipants. A limited budget will be available for travel support.

continued on next page

16 IRAM Info N°74

News and Events

The school web page and the registration form are available on the IRAM web site (Science Users > Events > IRAM schools). Links to the 2008 school pages, including

all presentations, are also provided. The deadline for registration is September 1st, 2010, but interested participants are encouraged to register as soon as possible,

since past experience suggests a rapid oversubscription.For any inquiry, please contact the organizing

committee at school2010@iram.fr

Observing with ALMA: Early Science 29th Nov. - 1st Dec. 2010by Frédéric Gueth

The IRAM node of the European ALMA Regional Center will organize a practical workshop on how to plan and analyze ALMA Early Science observations.

ALMA is currently in construction and should start full operations in 2013. However, already in 2011, ALMA will be operated with a limited number of antennas (16) and capacities (e.g. baselines < 1.5 km). The first Call for Proposals for this “ALMA Early Science” phase could be issued as early as the end of 2010, with a deadline in the first semester of 2011. To help the IRAM community to prepare this important milestone, the IRAM ARC node will be organizing a 3-days workshop on November

29th—December 1st 2010 at the institute’s headquarters (Grenoble, France).

The goal of the workshop is to provide the practical information needed to plan ALMA Early Science observations and answer the first Call for Proposals. A detailed, updated description of the ALMA Early Science capabilities will be presented: observing modes, correlator modes, system performances, calibration, etc. Practical points will be addressed, as e.g.

planning ALMA observations using the •available simulatorspreparing and submitting a proposal •using the ALMA Observing Tooldefining the instrumental setup for •

Phase 1 (proposals) and Phase 2 (accepted projects).

The workshop will include introduction and hands-on demonstration of key software for the ALMA users: the ALMA Observing Tool and the CASA off-line data reduction package.

About the WorkshopA web page and registration form will soon be posted on the IRAM site.

Interested participants can contact the organizing committee at:

alma2010@iram.fr.

Staff changes

Arrivals and DeparturesSince the last edition of the IRAM Newsletter, there have been a number of new hires and departures.

At the headquarters in Saint-Martin-d’Hères: Raymond Hennequin joined us in September 2009 to take the responsibility of the infrastructures’ unit.

Roberto Garcia Garcia joined the Back-End group in October 2009 to work on the numerical filtering of future spectrometers.

Three post-docs joined the Astronomy & Science Support group:

Yannick Libert to support observations at the Plateau de Bure, Francesco Fontani on a Marie-Curie Fellowship to work in the frame of the IRAM ARC-node and Math-ieu Lonjaret who came to work on ALMA software development.

In Granada, Manuel Gonzalez has joined the science operations group, on October 2009. His main work is to manage the HERA observing pools.

Two persons, who were present since the nearly beginnings of IRAM, departed at the end of 2009.

René Gontard, who was hired in 1986, retired after working for 23 years at the Plateau de Bure first as operator of the cable-car. He has maintained this position throughout the years (including the ‘blond-in’) and was, during the last years, in charge of maintening the departure station of the ‘blondin’ and the hangar in Montmaur.

He has been replaced by Julien Casali who has been hired as a technician working mainly at the observatory.

Gisela Matoso left IRAM after 21 years

Photograph showing Dr. Donald Snowstar who was temporarily hired in Saint-Martin-d’Hères from January 8th to January 15th, 2010 to the immense pleasure of the entire IRAM staff.

continued on next page

mailto:school2010@iram.frmailto:alma2010@iram.fr

February 2010 17

Staff changes

Publications

Title Authors Reference

A Spatially Resolved Inner Hole in the Disk Around GM Aurigae Hughes A. M., Andrews S. M., Espaillat C., Wilner D. J., Calvet N., D’Alessio P., Qi C., Williams J. P., Hogerheijde M. R.

2009, ApJ 698, 131

Low Milky-Way-Like Molecular Gas Excitation of Massive Disk Galaxies at z ~ 1.5

Dannerbauer H., Daddi E., Riechers D. A., Walter F., Carilli C. L., Dickinson M., Elbaz D., Morrison G. E. 2009, ApJ 698, L178

Wind measurements in Mars’ middle atmosphere: IRAM Plateau de Bure interferometric CO observations

Moreno R., Lellouch E., Forget F., Encrenaz T., Guilloteau S., Millour E. 2009, Icar 201, 549

Coupling of Microwave Resonators to Feed Lines Hammer G., Wuensch S., Roesch M., Ilin K., Crocoll E., Siegel M. 2009, ITAS 19, 565

Resolving the molecular environment of super star clusters in Henize 2-10 Santangelo G., Testi L., Gregorini L., Leurini S., Vanzi L., Walmsley C. M., Wilner D. J. 2009, A&A 501, 495

The modulation of SiO maser polarization by Jovian planets Wiesemeyer H. 2009, A&A 501, 647

A Millimeter-wave Interferometric Study of Dust and CO Disks Around Late Spectral Type Stars in Taurus-Auriga

Schaefer G. H., Dutrey A., Guilloteau S., Simon M., White R. J. 2009, ApJ 701, 698

Performance Improvement of a Flexible Telescope Through Metrology and Active Control

Greve A., Kärcher H. J. 2009, IEEEP 97, 1412

Search for corannulene (C20H10) in the Red Rectangle Pilleri P., Herberth D., Giesen T. F., Gerin M., Joblin C., Mulas G., Malloci G., Grabow J.-U., Brünken S., Surin L., Steinberg B. D., Curtis K. R., Scott L. T.

2009, MNRAS 397, 1053

Multiple low-turbulence starless cores associated with intermediate- to high-mass star formation

Beuther H., Henning T. 2009, A&A 503, 859

Multi-wavelength observations of the GRB 080319B afterglow and the modeling constraints

Pandey S. B., Castro-Tirado A. J., Jelìnek M., Kamble A. P., Gorosabel J., de Ugarte Postigo A., Prins S., Oreiro R., Chantry V., Trushkin S., Bremer M., Winters J. M., Pozanenko A., Krugly Y., Slyusarev I., Kornienko G., Erofeeva A., Misra K., Ramprakash A. N., Mohan V., Bhattacharya D., Volnova A., Plá J., Ibrahimov M., Im M., Volvach A., Wijers R. A. M. J.

2009, A&A 504, 45

Rotational structure and outflow in the infrared dark cloud 18223-3 Fallscheer C., Beuther H., Zhang Q., Keto E., Sridharan T. K. 2009, A&A 504, 127

S-bearing molecules in massive dense cores Herpin F., Marseille M., Wakelam V., Bontemps S., Lis D. C. 2009, A&A 504, 853

Radio Emission and Properties of Spitzer Selected Starbursts at z ~ 2 Omont A., Fiolet N., Polletta M., Owen F., Lonsdale C., Berta S., The Swimambo Collaboration 2009, ASPC 407, 142

Search for CO in Pluto’s and Triton’s Atmospheres Lellouch E., De Bergh C., Moreno R., Sicardy B., Käufl H. 2009, DPS 41, #06.08

The Thermal Emission of Comet 8P/tuttle Nucleus as Observed with the Plateau de Bure Interferometer

Boissier J., Bockelée-Morvan D., Groussin O., Biver N., Colom P., Crovisier J., Jorda L., Lamy P., Moreno R. 2009, DPS 41, #20.01

Radio-wavelength Investigations of Comet C/2007 N3 (lulin) Biver N., Bockelée-Morvan D., Colom P., Crovisier J., Gicquel A., Moreno R., Boissier J., Paubert G., Lis D. C., Dello Russo N., Vervack R. J., Weaver H. A.

2009, DPS 41, #23.05

Search for PH3 in the Atmospheres of Uranus and Neptune at Millimeter Wavelength

Moreno R., Marten A., Lellouch E. 2009, DPS 41, #28.02

Present and Future Cometary Science with the IRAM Plateau de Bure Interferometer

Boissier J., Bockelée-Morvan D., Biver N., Crovisier J., Moreno R., Lellouch E., Neri R. 2009, EM&P 105, 89

The Chemical Diversity of Comets: Synergies Between Space Exploration and Ground-based Radio Observations

Crovisier J., Biver N., Bockelée-Morvan D., Boissier J., Colom P., Lis D. C. 2009, EM&P 105, 267

C2H in prestellar cores Padovani M., Walmsley C. M., Tafalla M., Galli D., Müller H. S. P. 2009, A&A 505, 1199

Imaging Atomic and Highly Excited Molecular Gas in a z = 6.42 Quasar Host Galaxy: Copious Fuel for an Eddington-limited Starburst at the End of Cosmic Reionization

Riechers D. A., Walter F., Bertoldi F., Carilli C. L., Aravena M., Neri R., Cox P., Weiß A., Menten K. M. 2009, ApJ 703, 1338

Molecular Gas in Nearby Elliptical Radio Galaxies Ocaña Flaquer B., Leon S., Lim L., Dinh-v-Trung, Combes F. 2009, ASPC 408, 29

Feedback of AGN and SB Activity: Gas Chemistry and Excitation Conditions in the Centers of Nearby Active Galaxies

Krips M., Martin S., Neri R., Garcìa-Burillo S., Combes F., Petitpas G., Fuente A., Usero A. 2009, ASPC 408, 142

Molecular Gas in Ultra-Luminous Infrared QSOs Tan Q., Gao Y., Xia X. Y. 2009, ASPC 408, 179

The Nature of the Millimeter Bright Quasars at z ~ 6 Wang R., Carilli C. L., Neri R., Walter F., Bertoldi F., Cox P. 2009, ASPC 408, 452

Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530

Busquet G., Palau A., Estalella R., Girart J. M., Anglada G., Sepúlveda I. 2009, A&A 506, 1183

Search for cold debris disks around M-dwarfs. II Lestrade J.-F., Wyatt M. C., Bertoldi F., Menten K. M., Labaigt G. 2009, A&A 506, 1455

Intermittency of interstellar turbulence: extreme velocity-shears and CO emission on milliparsec scale

Falgarone E., Pety J., Hily-Blant P. 2009, A&A 507, 355

Methyl cyanide as tracer of bow shocks in L1157-B1 Codella C., Benedettini M., Beltrán M. T., Gueth F., Viti S., Bachiller R., Tafalla M., Cabrit S., Fuente A., Lefloch B. 2009, A&A 507, L25

90 GHz and 150 GHz Observations of the Orion M42 Region. A Submillimeter to Radio Analysis

Dicker S. R., Mason B. S., Korngut P. M., Cotton W. D., Compiègne M., Devlin M. J., Martin P. G., Ade P. A. R., Benford D. J., Irwin K. D., Maddalena R. J., McMullin J. P., Shepherd D. S., Sievers A., Staguhn J. G., Tucker C.

2009, ApJ 705, 226

First Redshift Determination of an Optically/Ultraviolet Faint Submillimeter Galaxy Using CO Emission Lines

Weiß A., Ivison R. J., Downes D., Walter F., Cirasuolo M., Menten K. M. 2009, ApJ 705, L45

Millimeter Observations of a Sample of High-Redshift Obscured Quasars Martìnez-Sansigre A., Karim A., Schinnerer E., Omont A., Smith D. J. B., Wu J., Hill G. J., Klöckner H.-R., Lacy M., Rawlings S., Willott C. J.

2009, ApJ 706, 184

of activity starting as secretary of the direc-tor and taking in 2003 the responsability of managing the logistics of the Plateau de Bure. This last task was a very difficult one that she always did with great efficiency and kindness.

She has been replaced by Cécile DiLeone, who learned directly from Gisela Matoso how to handle this critical job.

After ten years of editing the IRAM newsletter, Michael Bremer took over the

scientific responsability for the IRAM library. We thank him very much for the numerous issues of the newsletter that have kept the community informed!

from Sept. 2009 to Jan. 2010, compiled by Michael Bremer

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18 IRAM Info N°74

Publications

Title Authors Reference

Simultaneous Multi-Wavelength Observations of Sgr A* During 2007 April 1-11

Yusef-Zadeh F., Bushouse H., Wardle M., Heinke C., Roberts D. A., Dowell C. D., Brunthaler A., Reid M. J., Martin C. L., Marrone D. P., Porquet D., Grosso N., Dodds-Eden K., Bower G. C., Wiesemeyer H., Miyazaki A., Pal S., Gillessen S., Goldwurm A., Trap G., Maness H.

2009, ApJ 706, 348

Dissecting an intermediate-mass protostar. Chemical differentiation in IC 1396 N

Fuente A., Castro-Carrizo A., Alonso-Albi T., Beltrán M. T., Neri R., Ceccarelli C., Lefloch B., Codella C., Caselli P. 2009, A&A 507, 1475

Multi-wavelength properties of Spitzer selected starbursts at z ~ 2 Fiolet N., Omont A., Polletta M., Owen F., Berta S., Shupe D., Siana B., Lonsdale C., Strazzullo V., Pannella M., Baker A. J., Beelen A., Biggs A., De Breuck C., Farrah D., Ivison R., Lagache G., Lutz D., Tacconi L. J., Zylka R.

2009, A&A 508, 117

Deuterium chemistry in the Orion Bar PDR. “Warm” chemistry starring CH2D+

Parise B., Leurini S., Schilke P., Roueff E., Thorwirth S., Lis D. C. 2009, A&A 508, 737

The GISMO 2 Millimeter Camera Staguhn J. G., Benford D. J., Arendt R., Chuss D. T., Fixsen D., George J., Jhabvala C. A., Maher S. F., Miller T. M., Harvey Moseley S., Sharp E. H., Ungerechts H., Wollack E. J.

2009, AIPC 1185, 64

A Fast, Ultra-Sensitive and Scalable Detection Platform Based on Superconducting Resonators for Fundamental Condensed-Matter and Astronomical Measurements

Swenson L. J., Minet J., Grabovskij G. J., Buisson O., Lecocq F., Hoffmann C., Camus P., Villégier J.-C., Doyle S., Mauskopf P., Roesch M., Calvo M., Giordano C., Yates S. J. C., Baryshev A. M., Baselmans J. J. A., Benoit A., Monfardini A.

2009, AIPC 1185, 84

Infrared dark clouds as precursors to star clusters Rathborne J. M., Jackson J. M., Simon R., Zhang Q. 2009, Ap&SS 324, 155

Extragalactic CS Survey Bayet E., Aladro R., Martìn S., Viti S., Martìn-Pintado J. 2009, ApJ 707, 126

The Large Apex Bolometer Camera Survey of the Extended Chandra Deep Field South

Weiß A., Kovács A., Coppin K., Greve T. R., Walter F., Smail I., Dunlop J. S., Knudsen K. K., Alexander D. M., Bertoldi F., Brandt W. N., Chapman S. C., Cox P., Dannerbauer H., De Breuck C., Gawiser E., Ivison R. J., Lutz D., Menten K. M., Koekemoer A. M., Kreysa E., Kurczynski P., Rix H.-W., Schinnerer E., van der Werf P. P.

2009, ApJ 707, 1201

A search for neutral carbon towards two z = 4.05 submillimetre galaxies, GN20 and GN20.2

Casey C. M., Chapman S. C., Daddi E., Dannerbauer H., Pope A., Scott D., Bertoldi F., Beswick R. J., Blain A. W., Cox P., Genzel R., Greve T. R., Ivison R. J., Muxlow T. W. B., Neri R., Omont A., Smail I., Tacconi L. J.

2009, MNRAS 400, 670

A dry high altitude observatory in continental Europe Pérez E., Quesada J. A., Moles M., John D., Leon S., Ortìz J. L., Peñalver J. 2010, EAS 40, 119

The molecular gas content of the advanced S+E merger NGC 4441. Evidence for an extended decoupled nuclear disc?

Jütte E., Aalto S., Hüttemeister S. 2010, A&A 509, in press

A rotating molecular jet in Orion Zapata L. A., Schmid-Burgk J., Muders D., Schilke P., Menten K., Guesten R. 2010, A&A 510, in press

Circumstellar H I and CO around the carbon stars V1942 Sagittarii and V Coronae Borealis

Libert Y., Gérard E., Thum C., Winters J. M., Matthews L. D., Le Bertre T. 2010, A&A 510, in press

Spatially Resolved Molecular Gas Kinematics in a Lensed UV-Selected Galaxy at z = 2.26

Baker A. J., Lutz D., Tacconi L. J., Lin H., Allam S. S., Tucker D. L., Shapley A. E., Diehl H. T. 2010, AAS 41, 447

Hot-Dust, Star-Forming Ultraluminous Galaxies at High-Redshift Casey C. 2010, AAS 41, 533

Interferometric followup of CO (1-0) Detections with the Zpectrometer Sharon C. E., Baker A. J., Harris A. I., Seitz S., Tacconi L. J., Lutz D. 2010, AAS 41, 248

Characterizing non-axisymmetric Structure in Protostellar Envelopes Tobin J. J., Hartmann L., Bergin E., Looney L. W., Chiang H., Heitsch F. 2010, AAS 41, 255

Molecular Gas Properties of Early-type Galaxies Crocker A. F., Krips M., Young L. M., Bureau M., Combes F., Atlas3d Team 2010, AAS 41, 484

An Extremely Top-Heavy Initial Mass Function in the Galactic Center Stellar Disks

Bartko H., Martins F., Trippe S., Fritz T. K., Genzel R., Ott T., Eisenhauer F., Gillessen S., Paumard T., Alexander T., Dodds-Eden K., Gerhard O., Levin Y., Mascetti L., Nayakshin S., Perets H. B., Perrin G., Pfuhl O., Reid M. J., Rouan D., Zilka M., Sternberg A.

2010, ApJ 708, 834

Environment of MAMBO Galaxies in the COSMOS Field Aravena M., Bertoldi F., Carilli C., Schinnerer E., McCracken H. J., Salvato M., Riechers D., Sheth K., Smolcić V., Capak P., Koekemoer A. M., Menten K. M.

2010, ApJ 708, L36

MAMBO observations at 240GHz of optically obscured Spitzer sources: source clumps and radio activity at high redshift

Andreani P., Magliocchetti M., de Zotti G. 2010, MNRAS 401, 15

A new three-stage evolution model for millimeter to centimeter wavelength outbursts in BL Lacertae

Qian S.-J., Krichbaum T. P., Witzel A., Zensus J. A., Zhang X.-Z., Ungerechts H., Aller H. D., Aller M. F. 2010, RAA 10, 47

First attempt at interpreting millimetric observations of CO in comet C/1995 O1 (Hale-Bopp) using 3D+t hydrodynamical coma simulations

Boissier J., Bockelée-Morvan D., Rodionov A. V., Crifo J.-F. 2010, A&A 510, in press

Water Vapor in the Inner 25 AU of a Young Disk Around a Low-Mass Protostar

Jørgensen J. K., van Dishoeck E. F. 2010, ApJ 710, L72

High-precision astrometry with MICADO at the European Extremely Large Telescope

Trippe S., Davies R., Eisenhauer F., Schreiber N. M. F., Fritz T. K., Genzel R. 2010, MNRAS 402, 1126

High-molecular gaz fractions in normal massive star-forming galaxies in the young Universe

Tacconi L.G., Genzel R., Neri R., Cox P., Cooper M.C., Shapiro K., Bolatto A., Bouché N., Bournaud F., Burkert A., Combes F., Comerford J., Davis M., Förster Schreiber N.M., Garcia-Burillo S., Gracia-Carpio J., Lutz D., Naab T., Omont A., Shapley A., Sternberg A., Weiner B.

2010, Nature 463, 781