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251 — 8 November 2013 Editor: Bo Reipurth (Reipurth@Ifa.Hawaii.Edu) List of Contents THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar/planetary evolution and molecular clouds No. 251 — 8 November 2013 Editor: Bo Reipurth ([email protected]) List of Contents The Star Formation Newsletter Interview ...................................... 4 My Favorite Object ............................ 6 Editor: Bo Reipurth [email protected] Perspective ................................... 12 Technical Editor: Eli Bressert Abstracts of Newly Accepted Papers .......... 15 [email protected] Abstracts of Newly Accepted Major Reviews . 50 Technical Assistant: Hsi-Wei Yen Dissertation Abstracts ........................ 51 [email protected] New Jobs ..................................... 52 Editorial Board Summary of Upcoming Meetings ............. 54 Short Announcements ........................ 55 Joao Alves Alan Boss Jerome Bouvier Lee Hartmann Thomas Henning Paul Ho Cover Picture Jes Jorgensen Charles J. Lada This image shows the reflection nebula NGC 1579 Thijs Kouwenhoven located in the dark cloud L1482 at an approximate Michael R. Meyer distance of 700 pc. The nebulosity is illuminated Ralph Pudritz by the peculiar object LkHα 101, which is a heavily Luis Felipe Rodr´ıguez reddened massive star in a very early evolutionary Ewine van Dishoeck stage (seen as a faint optical star just south of the Hans Zinnecker brightest part of the reflection nebula). The figure is a composite of B-, V-, and R-band images, and The Star Formation Newsletter is a vehicle for covers approximately 6×7 arcmin, with north up fast distribution of information of interest for as- and east left. tronomers working on star and planet formation Image from G. H. Herbig, S. M. Andrews, & S. E. and molecular clouds. You can submit material Dahm, AJ, 128, 1233, 2004 for the following sections: Abstracts of recently accepted papers (only for papers sent to refereed journals), Abstracts of recently accepted major re- views (not standard conference contributions), Dis- sertation Abstracts (presenting abstracts of new Ph.D dissertations), Meetings (announcing meet- ings broadly of interest to the star and planet for- Submitting your abstracts mation and early solar system community), New Jobs (advertising jobs specifically aimed towards Latex macros for submitting abstracts persons within the areas of the Newsletter), and and dissertation abstracts (by e-mail to Short Announcements (where you can inform or re- [email protected]) are appended to each quest information from the community). Addition- Call for Abstracts. You can also submit via the http://www2.ifa. ally, the Newsletter brings short overview articles Newsletter web interface at hawaii.edu/star-formation/index.cfm on objects of special interest, physical processes or theoretical results, the early solar system, as well as occasional interviews. Newsletter Archive www.ifa.hawaii.edu/users/reipurth/newsletter.htm 2 . George Herbig (1920 – 2013) George Herbig passed away on October 12th at his home in Honolulu. He was the “father” of low-mass star formation studies, building the foundation upon which all of our current studies rest. A brief biography of George Herbig can be found at http://www.ifa.hawaii.edu/info/press-releases/Herbig/ A more detailed obituary will appear in Nature later this month. 3 star formation. What triggered that significant change of direction? Cecilia Ceccarelli A: For a not very romantic reason: the salary! I won a in conversation with Bo Reipurth permanent position at CNR in Italy to work in a group whose field of research was star formation. But I have to add that I instantaneously felt in love with this field, so different from the cosmology at the time, and not only for the subject, but even more for the methods. In cosmology, we had very few observations and lot of theories, whereas in star formation it was exactly the other way around, a lot of data and much less theory to explain them. Q: The protostar IRAS 16293-2422 has played an impor- tant role in your research, as it has for many other re- searchers. Do you think IRAS 16293-2422 is a special object, or in a special evolutionary stage, or is just very close and therefore more easily accessible? A: I think that this object has become a benchmark for astrochemistry studies in solar type protostars, mainly be- cause of its close distance but also because it has still a Q: You grew up and studied in Italy, but have made your relatively massive and extended envelope. It is clear that career in France, in Bordeaux and Grenoble. How did that young protostars can be different from IRAS16293-2422, come about, and was it an easy transition? for example we have the case of L1527 which shows a very different chemical composition. ALMA and NOEMA will A: It was not an easy transition, as I changed not only the certainly provide data on many other sources, which have country but also changed scientific direction, moving to as- been difficult to observe so far, and this will allow us to trochemistry and millimetre line observations, in addition understand whether and how IRAS16293-2422 is unique, to having two young kids (2 years old and one new born whether it is a special case as Orion is for high mass star baby). For all these reasons it took some time, but the formation. Laboratoire d’Astrophysique de Grenoble was welcoming and extremely fertile in ideas and competences, so things Q: You have taken a particular interest in deuteration, as were very much facilitated by that. I have also to say outlined in your major review for Protostars and Planets that I had the luck to meet Alain Castets, who introduced V. What have been your main insights, and where is that me to the field of astrochemistry and with whom I had a subject headed? great collaboration. The second person that played a huge A: In the 90s models did not predict the observability role in my transition was Emmanuel Caux at CESR (now of multiply deuterated molecules, which were thought to IRAP) in Toulouse. have a too low abundance. Our and others’ observations Q: What was your PhD about, and who were your most demonstrated that those theories were wrong. After more important early influences? than a decade we still have troubles in reproducing the ob- served abundances of doubly and triply deuterated molecules, A: My thesis was on cosmology, on the Cosmic Back- which means that something is still missing, even though ground Radiation field, and specifically on the Sunyaev- we have made huge progress. Two reasons make it im- Zeldovich effect. Although these topics are very far away portant to understand the origin of such a large molecular from my present field of research, I learned a lot during deuteration: (i) it provides us with very stringent con- that period. First of all I felt real enthusiasm for the re- straints on the pre-collapse phase of the relevant object search, I learned the necessary patience to obtain results and on its evolution; (ii) molecular deuteration provides a (my thesis was an experimental one, I worked on instru- sort of Ariadne’s thread that allows us to follow the history ments), and, last but not least, I realized the importance of the birth and early evolution of the Solar System. With of intuition, to understand and explain with simple ideas respect to this last point, we are preparing together with even very complex problems. I think that this was the six other colleagues who are experts in comets, meteorites great education I received from my supervisor, Francesco and Solar Nebula models, a chapter for the PP VI book Melchiorri. on the deuteration across the star and planet formation Q: So up until 1986 you worked on extragalactic astron- process, from the very first pre-collapse phase up to the omy and the cosmic microwave background, and suddenly formation of the terrestrial oceans. you saw the light and switched to the earliest phases of 4 Q: You have extensively used data from ISO. How impor- viding us with plenty of information on their content in tant was ISO, and what do you see as the major legacy of terms of water and many other species, many of which that satellite? are not detectable with groundbased telescopes. Notable A: After IRAS, which provided us with the list of IR examples are the deuteration of water in different objects, sources in the sky, ISO was the first observatory in the including a shock spot caused by a molecular outflow, the FIR. It allowed us to study the IRAS sources (and more), mysterious chlorine chemistry – we haven’t understood so making maps, SEDs and, even more innovative, high to far where chlorine is as just a little fraction is observed in moderate resolution spectra in the IR to FIR. It was a rev- the gas phase even in sites where it should be all gaseous olution in several fields, from the studies of the ices to the –, the nitrogen chemistry, also very poorly understood. line spectra of galactic and extragalactic objects, which Q: You have an important leadership role as the head of the allowed us to understand the gas cooling mechanisms and AstroMol group in Grenoble. With cutbacks everywhere, the distribution of the oxygen, the most abundant element do you still encourage young people to enter science and after hydrogen and helium, in molecules, including water. get a PhD in molecular astronomy? The importance of ISO is testified by the large number of A: I have left the leadership of the group to my colleagues published articles and by the fact that new articles with since a while. At present, Bertrand Lefloch is the very ap- ISO data are still being published! preciated group leader. But I’m still engaged in promoting Q: Your most-cited paper deals with far-infrared line emis- molecular astronomy, I teach and regularly propose PhD sion from collapsing protostellar envelopes.
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