School of Physics, Main Building (K14 on linked map)
UNSW is 15 minutes by taxi (and about $25) from Sydney's Kingsford Smith airport, and a similar distance south of the city centre, in Sydney's Eastern Suburbs. See the Google Map.
This workshop is the yearly meeting of the NANTEN2 consortium. NANTEN2 is a 4m sub-millimetre wave telescope operating at the 4,800m Pampa La Bola on the Atacama plateau of Northern Chile (a part of the ALMA site). It is run by a 6-nation university consortium, led by the University of Nagoya in Japan and the University of Cologne in Germany, and including members in Chile, South Korea and Switzerland, as well as Australia. NANTEN2 will be equipped with dual-frequency, 8-element array receivers, operating at frequencies of 460/492 and 806/892 GHz. The principal scientific programs will involve mapping of the Galaxy and the Magellanic Clouds in the excited CO J=4-3 and 7-6 lines and the two [CI] lines emitting in these frequency bands. At 500 GHz its beamsize is similar to the 22m Mopra telescope operating in the 100 GHz band, lending itself to complementary observations of higher excitation molecular lines that Mopra can map in the ground state lines.
Australia's participation in NANTEN2 has been made possible by an ARC LIEF grant, awarded this year to UNSW, Sydney and Macquarie universities.
The workshop will have two primary purposes. The first is to discuss operational matters relating to the telescope. The second is to discuss the telescope's scientific program. With the complementarity to Australia's millimetre-wave facilities there are many opportunities for scientific collaborations. The local participants are keen to extend this opportunity to the wider community, and not just have it confined to the three participating Australian universities in the consortium. We are therefore opening the meeting to the Australian astronomy community. In particular, if you would like to make a presentation to describe a prospective science program, please let us know.
There is not a formal program to this meeting. The first day will be largely devoted to operational matters within the consortium, and is likely only to be of interest to the consortium members. The second day will include discussion on the future science program. It will include a few short presentations on prospective projects. We will publish a program closer to the event.
We also intend organising a social event for the Wednesday June 13, primarily for our overseas guests. It will involve a tour and bushwalk in national parks by the Hawkesbury River, to the north of Sydney. Let us know if you're interested in participating.
For members of the NANTEN2 collaboration. Meet in the lobby of the Coogee Sands Hotel at 6pm and we will head to a nearby venue.
First Year Laboratory Annexe, School of Physics, UNSW
Start time 9:30am
Since this is a public holiday the entrances to the School of Physics will be locked. Please enter by the entrance in the courtyard near the First Year Laboratory, as in the map below. We will endeavour to pick people up from Coogee Beach at ~9am – details to be sorted out on Sunday night.
12:30pm Lunch in Meeks Cafe (9663-4495)
7pm NANTEN2 Collaborators Dinner in Coogee (Tropicana Cafe, 207 Coogee Bay Road, 02-9665-5619)
Common Room (Room 64), School of Physics, UNSW
Start time 9:30am
The speakers are:
| Time | Speaker | Title |
| 9:30am | Michael Burton | Welcome |
| 9:40 | Toshikazu Onishi | An overview of NANTEN2: I the telescope and observatory |
| 10:00 | Robert Simon | An overview of NANTEN2: II site statistics, prospective science, surveys with SMART |
| 10:20 | Norikazu Mizuno | First results from NANTEN2: the LMC & SMC |
| 10:35 | Juergen Stutzki | First results from NANTEN2: excitation in the LMC and nearby galaxies |
| 10:50 | Annie Hughes | The LMC as seen by Mopra |
| 11:05 | Erik Muller | Opportunities in the LMC-SMC Bridge |
| 11:20 | All | Coffee Break |
| 11:45 | Yasuo Fukui | First results from NANTEN2: the Galactic centre region |
| 12:00 | Paul Jones | The Central Molecular Zone |
| 12:15 | Gavin Rowell | TeV gamma-ray astronomy and connections with molecular clouds studies |
| 12:30 | Robert Simon | First results from NANTEN2: galactic high mass star formation (Carina, NGC 3603, Rosette) |
| 12:45 | Kate Brooks | Some thoughts on Carina |
| 13:00 | All | Lunch Break (JGs cafe on campus) |
| 14:00 | Maria Cunningham | Star formation in G333 triggered by dynamic feedback |
| 14:15 | Motosuji Fujishita | First results from NANTEN2: yet more results! |
| 14:30 | Juergen Stutzki | Analysis tools, modelling the emission of the Milky Way with clumpy PDR models |
| 14:45 | Frank Bensch | B68: a benchmark for spherical PDR models |
| 15:00 | Michael Burton with Andrew Walsh and Steven Longmore | Uncovering the earliest stages of massive star formation (including the Mopra HOPS survey, ammonia and HCHIIs) |
| 15:20 | Peter Barnes | CHAMP - the Census High And Medium-mass Protostars |
| 15:30 | All | Tea Break |
| 16:00 | Open Discussion | Observing programs for NANTEN2 Complementary millimetre-wave observations from Australia Other necessary observations and investigations |
| 17:15 | All | Close |
| From ~6pm | All | Workshop drinks and dinner, likely to be in the Coogee Bay Hotel |
A tour of some of the scenic highlights along the mighty Hawkesbury River, to the north of Sydney, including possible bush walks into the national parks – a journey back in time! Please let us know if you are interested in participating, including whether you can offer transportation.
Please register by following this link if you wish to attend the meeting. Let us know if you would like to give a talk when you register.
The following have indicated their interest in attending the meeting.
| Peter Barnes | U Sydney |
| Indra Bains | U Swinburne |
| Frank Bensch | U Bonn |
| Kate Brooks | ATNF |
| Michael Burton | UNSW |
| Maria Cunningham | UNSW |
| Joanne Dawson | Nagoya U |
| Motosuji Fujishita | Nagoya U |
| Yasuo Fukui | Nagoya U |
| Urs Graf | U Koln |
| Annie Hughes | U Swinburne |
| Balt Indermuehle | UNSW |
| David Jones | U Adelaide |
| Paul Jones | UNSW |
| Steve Longmore | UNSW |
| Sarah Maddison | U Swinburne |
| Norikazu Mizuno | Nagoya |
| Erik Muller | ATNF |
| Toshikazu Onishi | Nagoya U |
| Gavin Rowell | U Adelaide |
| Martin Saul | UNSW |
| Robert Simon | U Koln |
| Juergen Stutzki | U Koln |
| Chris Wright | UNSW ADFA |
Parking is available on the top floor of the Barker Street multi-storey car park (enter UNSW via Gate 14). It is metered and you need to obtain a parking ticket from the machines nearby - bring some change along! The 891 Express bus connects UNSW with Central Station in ~20 minutes.
Attendees are responsible for making any accommodation arrangements. However we can make some recommendations for you. Coogee beach (Coogee Bay on the map below) is about 30 minutes walk from UNSW, or 10 minutes by bus or 5 minutes by taxi. Please also note that this is a holiday weekend in Sydney (the Queen's Birthday holiday weekend!) with Monday June 11 being a public holiday. Hotels may thus book up quickly for the Sunday and Monday nights.
161-167 Dolphin Street in Coogee. On beautiful Coogee Beach. Rates $145/night for deluxe standard studio, $165 for deluxe courtyard studio, $195 for deluxe ocean view studio and $180 for one-bedroom apartment. Book by emailing Karen Chow, the marketing manager, on karen@coogeesands.com.au and mentioning 'NANTEN2'. Telephone 1800-819-403 (toll free) and 02-9665-8588.
A boutique hotel also on Coogee Beach. Rates $148.50/night for standard room, $162 for standard king room, $189 for superior king room, $189 for balcony room, $225 for ocean view room and $252 for superior ocean view room (these are a 10% discount). Email the Dive Hotel at thedive@bigpond.com.au for reservations, quoting the UNSWNANTEN2 reference and asking for the discount. 234 Arden Street, Coogee, NSW 2034. Telephone: +61 2 9665 5538.
A cheaper option in Randwick, half way between Coogee Beach and UNSW. Rates about $100 per night. Email randwicklodge@bigpond.com. 211 Avoca Street, Randwick, New South Wales 2031, Phone: (61) (2) 9310 0700.
Convenient to UNSW (just across the road from the School of Physics) but otherwise not much to recommend it. Rates from $135 night (single) and $150 night (double, twin). Email reservations@barkerlodge.com.au and mention the School of Physics. Address 32 Barker Street, Kingsford NSW 2032. Tel (02) 9662 8444.
There are plenty more options for Sydney accommodation available from the web, eg at http://www.sydneyhotelsaccommodation.com/
Frank Bensch - B68 as test case for a PDR in the diffuse galactic radiation field
The dark globule B68 is an example which might serve as a test object for a PDR model in a weak external FUV field. The density profile of B68 is very well known and its symmetry is well matched to a spherically-symmetric PDR model. The present study compares the KOSMA-tau PDR model to observations of the lowest transition in 12CO, 13CO(3-2) and (2-1), as well as the cloud-averaged [CI] 3P1-3P0 line intensity. The impact of CO depletion, PAHs in the chemical network, as well as variations in the external FUV field are studied. We find it difficult to simultaneously match the observed 12CO and 13CO emission. A model which matches the observed 12CO observations and the cloud-averaged [CI] intensity gives 13CO intensities which are too large by a factor of 2-3. A steep drop in the line excitation seems to be required from the region traced by 12CO to the (somewhat deeper) layer traced by the 13CO transitions. This model allows us to predict the intensity distribution and line profiles of the 12CO, 13CO rotational transitions and both [CI] fine-structure lines, and thus can be tested with NANTEN2. The spectral line data and the results of the NANTEN2 observations made with the KOSMA 490/810 GHz test receiver during the 2006 observing campaign are presented, and the prospects of future observations are discussed.
Kate Brooks – Some thoughts on Carina
The Carina Nebula (NGC 3372) is our richest nearby laboratory in which to study feedback through UV radiation and stellar winds from very massive stars during the formation of an OB association, at an early phase in the evolution of the surrounding proto-superbubble, before supernova explosions have disrupted the environment.?In Carina, this feedback is triggering successive generations of new star formation around the periphery of the nebula, while simultaneously evaporating the gas and dust reservoirs out of which young stars are trying to accrete material. In this talk I will provide a census of the Carina nebula and put forward ideas for future projects with Mopra and NANTEN2.
Michael Burton - Astronomy on the Altiplano - sub-millimetre wave astronomy from the Atacama plateau of Chile
The altiplano is a 5000m elevation plateau in the Andes of South America where are found the driest temperate-latitude places on the Earth. This provides superb conditions for sub-millimetre wave astronomy, opening up new windows for observation through that are inaccessible from other temperate sites. In these wavebands emission from dust and molecules is prominent, including the birth sites of massive stars in our own Galaxy and the red-shifted emission from some of the youngest galaxies in the Universe.
The altiplano nearby to the town of San Pedro de Atacama in Chile is about to become home to the largest concentration of front-line telescopes on our planet. While the billion-dollar ALMA (the Atacama Large Millimetre Array) project is well known, there are eight other telescopes at various stages in their planning and construction processes. These range from the 4m NANTEN2 telescope to the 25m CCAT (Cornell Caltech Atacama Telescope). Three Australian universities (UNSW, Sydney, Macquarie) have recently joined the international university consortium building the NANTEN2 sub-millimetre wave telescope.
This talk will provide an introduction to the Atacama plateau, and in particular to the NANTEN2 telescope. It will discuss some of the science opportunities they present, and their complementarity to capabilities of Australia's own millimetre-wave facilities.
Michael Burton - Uncovering the earliest stages of massive star formation
We outline a program to uncover the sites of conception for massive star formation, and how the environment may be studied using molecular lines probes. It builds on the methanol maser multibeam survey now underway with Parkes. Mopra and NANTEN2 feature prominently, as does APEX and ATCA. The program also will serve to feed ALMA, providing the most interesting sources to be imaged in all the gory detail that ALMA will facilitate.
Maria Cunningham - Star formation in G333 triggered by dynamical feedback?
The Mopra telescope has been used to map a 1.2 x 0.6 degree region of the southern Galactic plane in rotational transitions of 20 different molecules. The survey, made possible by the wide bandwidth and high spectral resolution capabilities of the new MOPS receiver, has produced a unique data-set that is being used to give new insights into the dynamics and chemistry of the interstellar medium.
Here we present some highlights of the results, showing how combinations of molecules can be used to trace dynamical structures such as molecular shells, outflows and gas filaments, and how these are related to star formation activity within the region. For example, the molecule N2H+ seems to be a surprisingly good tracer of shell-like structures within the G333 cloud. This molecule is generally found to trace cool, dense quiescent gas, and in this case seems to be tracing gas compressed by the shock front of an expanding shell. In some places the shells have begun to fragment and form dense cores, leading us to conclude that within the G333 region star formation is often triggered by dynamical feedback.
We also discuss the role that the NANTEN2 telescope can play in following up the structures we have identified. The similar beam-size at of NANTEN2 at sub-millimetre wavelengths to Mopra at 3 mm will allow NANTEN2 observations of higher energy molecular transitions to be compared with the lower energy transitions from Mopra, from which the temperature and density of the gas can be inferred.
Paul Jones - The Central Molecular Zone near the Galactic Centre
We are studying of the Central Molecular Zone (CMZ) in the inner few degrees around the Galactic Centre, with the Mopra telescope using the new capabilities of the MOPS digital filter bank.
In 2006 'pilot' observations we mapped a 5 x 5 arcmin area of the Sagittarius B2 molecular cloud complex. This covered nearly all of the 83.5 to 113.5 GHz frequency range with 4 tunings of the 8 GHz wide-band mode to image over 150 spectral lines, and we also observed 24 of these lines with the zoom mode (3 tunings) at higher velocity resolution. This shows substantial differences in chemical and physical conditions within the complex. The coverage is now (mid 2007) being extended to the 0.3 deg x 1.1 deg area including Sgr A and Sgr B2, between 85.3 and 93.3 GHz. We intend, in later winter seasons, to extend the frequency and longitude coverage.
Gavin Rowell - TeV gamma-ray astronomy and connections with molecular cloud studies
TeV gamma-rays are the most accessible tracer of multi-TeV particle acceleration in the Universe. In combination with studies that trace molecular clouds, we can determine the likelihood that TeV gamma-ray sources are the result of acceleration hadrons or cosmic-rays. The origin of cosmic rays (Galactic and extragalactic) is one of the oldest questions in astrophysics. I will briefly summarise recent relevant results, developments in TeV gamma-ray astronomy and future plans.
An Overview of NANTEN2, in two parts
Toshikazu Onishi – I: The Telescope and Observatory
Robert Simon – II: Site statistics, prospective science, surveys with SMART
These talks will give a brief introduction to the NANTEN2 telescope and observatory, as well as to NANTEN science in the framework of other observations of the southern Milky Way. It will set the stage for the later presentations of the first science results and the discussion on future projects and collaborations.
Talk I will discuss NANTEN2 as part of astronomy activities in Chile, the telescope characteristics, and overview the Nagoya receivers and science plans. Talk II will briefly summarise the ALMA site statistics and the impact on observing at the highest frequencies. It will then give an overview of the potential NANTEN2 science with particular emphasis on the highest observing frequencies covered with the SMART receiver, high mass star formation, and PDRs.
Robert Simon – First results from NANTEN2 - Galactic high mass star formation
In this talk, I will give a short summary of the first results for Carina, NGC 3603, and the Rosette. I will use the Carina results as a template to show what one can do in terms of analysis and interpretation of NANTEN2 data within the framework of clumpy PDRs.
Juergen Stutzki - First results from NANTEN2 – Excitation in the LMC and nearby galaxies
In this talk, I present the results from the NANTEN2/test-receiver commissioning period in the fall of 2007 obtained in the Circinus and NGC 4945 and the LMC N159W complex. I discuss the excitation conditions that can be derived from the observed sub-mm CO and [CI] lines.
Juergen Stutzki - Analysis tools, modelling the emission of the Milky Way with clumpy PDR models
This talk will present a short overview of an important tool for the interpretation of PDR line emission: a clumpy PDR model, which is based on the KOSMA-tau spherical clump PDR code, combined with appropriate averaging over a clump distribution. The clump ensemble is assumed to have a power-law mass and mass-size distribution. The model thus incorporates both the physical and chemical conditions predicted in photon dominated regions with an adequate treatment of the observed characteristics of the complex structure of the dense interstellar medium.
As one application of the model, I present its predictions for the global sub-mm and FIR line emission of the Milky Way and compare this with the COBE data set.
Michael Burton, 05/06/07