stth

21 -26 August
University of Exeter
Programme

2

Contents
Page No.
LOC and SOC members

4

Conference programme

5-8Social events

9

Molecular clouds talk abstracts (Monday)

11-20

Protostellar cores talk abstracts (Tuesday)

21-28

Splinter sessions (Wednesday)

29-34

Young clusters & protostars talk abstracts (Thursday)

35-42

Discs talk abstracts (Friday)

43-50

Poster submissions

51-62

Delegate list

63-68

3

Local Organising Committee (University of Exeter)
Tim Harries
Chris Brunt
Emma Way
Ana Duarte Cabral
Pablo Loren Aguilar
Tom Douglas
Sam Morrell
Martyn Brake

You can contact us at any time throughout the conference at: sf2016@astro.ex.ac.uk

Scientific Organising Committee
Philippe André, CEA-Saclay, France
Crystal Brogan, NRAO, USA
Chris Brunt (Co-Chair), University of Exeter, UK
Cathie Clarke, University of Cambridge, UK
Janet Drew, University of Hertfordshire, UK
Kees Dullemond, University of Heidelberg, Germany
Tim Harries (Co-Chair), University of Exeter, UK
Lynne Hillenbrand, Caltech, USA
Shu-ichiro Inutsuka, Nagoya University, Japan
John Monnier, University of Michigan, USA4

08:30
08:50

0900

0940

1020

1040

1100

Monday 22 August
Tuesday 23 August
Molecular clouds
Protostellar cores
Coffee/tea & mini pastry
Tim Harries & Chris Brunt
Welcome address

Tim Harries & Chris Brunt
Notices & updates

Stefanie Walch(University of Cologne)
Theory review

Kengo Tomida(University of Osaka)
Theory review

Nicolas Peretto(University of Cardiff)
Observational reviewAnaëlle Maury(CEA/Saclay)
Observational review

Masato Kobayashi(Nagoya University)
Evolutionary Picture of
Giant Molecular Cloud
Mass Functions on
Galactic Scales

Vera Könyves (CEA/Saclay)
A census and properties ofdense cores and filamentsin the Aquila and Orion B
cloud complexes

Andrea Bracco(CEA, Saclay)
The relative orientation
between magnetic fields
and filamentary density
structures from the diffuse
ISM to molecular clouds

Alana Rivera-Ingraham(ESA)
Extreme Star Formation in
the Galaxy: The Herschel
View

Coffee break

Wednesday 24 August
Coffee/tea & mini pastry
Splinter sessions will takeplace from 0900 – 12:00.

Kraus(Planet Formation Imager)
Forum seminar room 4
Bell(The ages of young stars)
Forum seminar room 6
Hatchell(Measuring temperaturesand densities in starformation regions)
Forum seminar room 10
Goodwin(Computational starformation)
Forum seminar room 5
Brunt(Early-career researchers)
Alumni Auditorium, The
Forum

Thursday 25 August
Friday 26 August
Protostars & clusters
Discs
Coffee/tea & mini pastry
Tim Harries & Chris Brunt
Notices & updates

Tim Harries & Chris Brunt
Notices & updates

Nick Wright(University of Keele)
Observational review

Catherine Espaillat(Boston University)
Observational review

Stella Offner(UMass Amherst)
Theory review

Richard Alexander(University of Leicester)
Theory review

Richard Parker(Liverpool John Moores
University)
The initial conditions ofstar formation from spatial
and kinematic
substructure

Tim Naylor(University of Exeter)
A Dynamic ColourMagnitude Diagram for
the Orion Nebula Cluster

Isabelle Baraffe(University of Exeter)
Consistent models of
accretion history andmulti-dimensional
structure of accreting
young stars.

Kenny Wood
(University of St. Andrews)
A Model for (Quasi-)
Periodic Multi-wavelength
Photometric Variability in
Young Stellar Objects

Coffee break1150

Monday 22 August
Molecular clouds
Simon Glover(Heidelberg University)
Hunting for observationalsignatures of molecular
cloud formation

Tuesday 23 August
Protostellar cores
Isabelle Ristorcelli(IRAP / CNRS UPS
Toulouse)
A statistical analysis ofpolarized dust emission in
the environment of Planck
Galactic cold clumps
Jenny Hatchell(University of Exeter)
Taking the temperature of
local star-forming clouds
with the JCMT Gould Belt
survey1210

Ana Duarte Cabral(University of Exeter)
Observing simulations:
Molecular clouds and theirjourney in the Galaxy

1230

Eric Keto(Harvard-Smithsonian
Center for Astrophysics)
A simple description of theenergy budget inmolecular clouds and their
atomic envelopes

Sarah Sadavoy (MPIA)
Dust Emissivity in OMC
2/3: Linking the Diffuse
Cloud to the Dense Cores

Volker Ossenkopf-Okada(University of Cologne)
Column density PDFs as adiagnostic tool

Chris Wright (UNSW)
Magnetic fields via
thermal infrared
polarimetric imaging

1250

1310

Thursday 25 August
Protostars & clusters
Laura Venuti (INAF)
Variety of accretion
regimes in the young open
cluster NGC 2264
Packed lunches will beavailable for collection
from Holland Hall at 12:00.
Alicia Aarnio(University of Michigan)
Assessing MagnetosphericAccretion in Herbig Ae/Be
Stars

Coaches for the afternoon
excursions will leave
Holland Hall promptly at
13:00.

Lunch

Friday 26 August
Discs
Gilles Chabrier(NS-Lyon & Exeter)
Formation of proto-stellar
and proto-planetary disks
in star formation: the key
roles of different physicalmechanisms
Alvaro Ribas(Boston University)
Protoplanetary disk
lifetimes in nearby starforming regions

Carlo Manara (ESA/ESTEC)
Disk evolution in young
clusters: accretion, winds,
and dynamical propertiesof young stars and their
disks

Melissa K. McClure (ESO)
T Tauri disk gas masses
measured from hydrogen
deuteride

Philip Lucas(University of Herts)
A population of eruptive
variable protostars in VVV

Stefan Kraus(University of Exeter)
Resolving the discstructure of FU Orionis
stars

Lunch

6

1440

1500

1520

1540

1600

Monday 22 August
Molecular clouds
Seamus Clarke(Cardiff University)
Fragmentation ofaccreting filaments
Jouni Kainulainen(Max-Planck-Institute for
Astronomy)
Fragmentation of theIntegral Shaped Filamentin Orion A as viewed by
ALMA
Kate Pattle (UCLAN)
First results of the JCMTBISTRO survey: The
magnetic field of Orion A

Huei-Ru Vivien Chen(National Tsing Hua
University)
Filamentary Accretion
Flows in the IRDC M17
SWex

Tuesday 23 August
Protostellar coresBenoît Commerçon(CRAL ENS Lyon)
Outflows and disks
formation in massive corescollapse
Yusuke Aso(University of Tokyo)
ALMA observations of
Keplerian disks aroundprotostars

Wednesday 24 August

Excursions: Jurassic Coast Pebblebed
vineyard Dartmoor hike

Ben Lewis(University of Exeter)
Shaken and stirred - therole of turbulence,magnetism and radiationin the formation of
protostars.
Neil Vaytet(University of
Copenhagen)A grid of 1D low-mass starformation collapse
models: not all dense
clouds form first Larson
cores

Thursday 25 August
Protostars & clusters
Matthew Bate
(University of Exeter)
The dependence of stellar
properties on metallicity
Tom Megeath(University of Toledo)
Low Mass Star Formationin the DIverse
Environments of Orion:
Result from the HerschelOrion Protostar Survey
Jan Forbrich(University of Vienna)
The Orion Radio All-Stars:
new perspectives in stellar
radio astronomy

Nadia Murillo(Leiden University)
Do siblings always formand evolve at the sametime? Coevality of multiple
protostellar systems with
Herschel

Tea breakFriday 26 August
Discs
Katharine Johnston(University of Leeds)
A Keplerian-like discaround the forming O-typestar AFGL 4176
James Owen (Princeton)
Vortices from low-massplanet formation intransition discs

Michael Ireland (ANU)High Angular Resolution
Mid-Infrared Imaging ofTransitional Disks

Pablo Loren-Aguilar(University of Exeter)
Toroidal vortices as asolution to the dust
migration problem

Tea break

7

1650

1710

1730

1750

Monday 22 August
Molecular clouds
Jonathan Henshaw(Liverpool John Moores
University)
Seeding the Galactic
Centre gas stream: initialconditions for theformation of Young
Massive Clusters
Joao Alves(University of Vienna)
Blue Streams and local starformation

Tuesday 23 August
Protostellar cores
Yusuke Tsukamoto(RIKEN)
Bimodality of Circumstellar
Disk Evolution Induced by
the Hall Current

Thursday 25 August
Protostars & clusters
Megan Reiter(University of Michigan)Powerful jets driven byintermediate-mass
protostars in the Carina
NebulaFriday 26 August
Discs
Giovanni Rosotti(University of Cambridge)
What is the minimum
planet mass that createsobservable signatures inproto-planetary discs?

Oliver Lomax(University of Cardiff)Core fragmentation andprotostellar multiplicity

Guido De Marchi (ESA)The Tarantula of low-massstars

Eiji Akiyama (NAOJ)
Differential Grain Growthin the Spiral Structure of
the LkHa 330 Disc

Emily Drabek-Maunder(Imperial College London)
The JCMT Gould Belt
Survey: Understanding theinfluence of molecular
outflows on Gould Belt
clouds
Enrique VazquezSemadeni (RyA-UNAM)
Core structure andevolution in globally
collapsing molecular
cloudsJoana Oliveira(University of Keele)
Herschel Spectroscopy of
Massive Young Stellar
Objects in the Magellanic
CloudsLee Hartmann(University of Michigan)
Mass functions of starclusters and the uppermass stellar IMF.

John Monnier(University of Michigan)
GPI observations of Herbig
Ae/Be stars

Joseph Mottram (MPIA)
Fragmentation and disk
formation in high-massstar formation

Philippe André(CEA/Saclay)
The role of interstellar
filaments in the origin of
the stellar initial massfunction

Conference summary8

Lee Hartmann(University of Michigan)

Social Events
Sunday 21st August

Welcome drinks reception and buffet, Holland
Hall

19:00

Monday 22nd August

Poster session and drinks reception, The Forum

18:10 – 19:00

Tuesday 23rd August

Barbeque, Holland Hall

19:00

One free drink ticket for all delegates
A cash bar will be available (credit/debit cards
will not be accepted)
Wednesday 24th August

Afternoon excursions
Packed lunches will be available for collectionat Holland Hall from 12:00

Thursday 25th AugustJurassic Coast Tour (2 coaches)

Dartmoor Hiking Tour (2 coaches)Pebblebed Vineyard

Conference dinner, the Great Hall

Coaches leave from
Holland Hall at 13:00
prompt

19:00

Starting with a drinks reception and followed
by a three course meal. After the meal we will
be entertained by the Soul Traders with a mixof soul, funk and rock ‘n’ roll.
A cash bar will be available (credit/debit cards
will not be accepted).
Friday 26th August

Public Talk, Alumni Auditorium, The Forum
Mark McCaughrean: ESA’s Big Year in Space
Science 2016
The talk will be preceded at 18:10 by drinks andnibbles for delegates on the Forum mezzanine

19:00

Monday 22nd August

Molecular Clouds
Talk Abstracts

11

Time of talk: Monday 09:00
Name: Stefanie Walch
Organisation: University of Cologne
Title: Theory review
Abstract:
Molecular clouds condense out of the warm interstellar medium (ISM) on scales of several 100 pc and hostfilamentary substructures on sub-pc scales. Furthermore, molecular clouds (MCs) consist of molecular hydrogen(H2), which can only be traced indirectly in observations, mostly by means of CO line and dust extinction
measurements. Since they are observed to host large non-thermal line widths, the cloud sub-structure seems to
be shaped by supersonic turbulence. The crux, however, is that supersonic turbulence is expected to decay in acrossing time unless it can be sustained by some physical process, e.g. stellar feedback. Since the turbulent
dynamical state has been observed, the idea of short-lived, dynamically evolving MCs is widely accepted. It isthus likely that the turbulent, internal sub-structure of MCs is imprinted already during their formation process.
In this talk I will review the current theoretical understanding of molecular cloud formation and evolution. A 30minute review of molecular clouds from a theoretical perspective.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 09:40
Name: Nicolas Peretto
Organisation: Cardiff University
Title: Observational review
Abstract:
The past few years have seen a great deal of spectacular large-scale surveys of star-forming regions across the
Galaxy with unprecedented sensitivity and angular resolution. Combined with state-of-the-art interferometricfollow-up observations, these surveys are transforming our view and understanding on how interstellar matteris transferred from large diffuse atomic clouds to compact protostellar objects. In this talk, I will review some of
the key observational results of the past five years, focussing on the formation, evolution, and fragmentation ofinterstellar filaments into cores. Tightly related issues such as the formation of molecular clouds, the starformation efficiency, and the importance of feedback will be briefly addressed.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 10:20
Name: Masato Kobayashi
Organisation: Nagoya University
Title: Evolutionary Picture of Giant Molecular Cloud Mass Functions on Galactic Scales
Abstract:
We formulate and compute the time evolution of giant molecular cloud mass functions on galactic disks. In ourmodel, a network of expanding supernova remnants and HII regions drives the giant molecular cloud formationand evolution. Such a network provides (i) giant molecular cloud formation and self-growth through multiple
episodes of warm neutral medium compression, (ii) giant molecular cloud self-dispersal by radiation frommassive stars that are born within those clouds, and (iii) cloud-cloud collisions. Our formulation reflects thesethree phenomena by coarse-graining them typically over 10 Myrs. We successfully reproduce the observed
variation of giant molecular cloud mass functions between arm and inter-arm regions (e.g., M51 by Schinnerer

12et al. 2013; Colombo et al. 2014a). Our results suggest that the mass function slope is controlled by the ratio of
giant molecular cloud formation timescale over its dispersal timescale, whereas the massive end is controlled
by cloud-cloud collisions. Future large radio observations with finer spatial resolution and higher sensitivity canobserve giant molecular clouds with much lower mass than before, which may put unique constraints on thegiant molecular cloud formation/dispersal timescales in different environment on galactic scales. In addition,
our results also suggest that some amount (typically a few per cent) of dispersed gas is consumed to form anewer generation of giant molecular clouds. Therefore, we insist that, obtaining a complete picture of gas
recycling processes in interstellar medium requires the understanding of the fate of dispersed gas such as COdark clouds and optically thick HI gas, which thus needs massive magnetohydrodynamics simulations. In thiscontribution, we would like to present our results and discuss this new unified picture of giant molecular cloudmass function evolution throughout galactic disks.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 10:40
Name: Andrea Bracco
Organisation: CEA, Saclay
Title: The relative orientation between magnetic fields and filamentary density structures from the diffuse ISM
to molecular clouds
Abstract:
Investigating the dynamics of the interstellar medium (ISM) is key to gaining insight into the formation of starforming filaments in molecular clouds (MCs). A plethora of numerical and analytical models associate the originof this filamentary structure to the interplay between self-gravity and magnetohydrodynamical (MHD)
turbulence in the ISM. However, only few observational constraints exist to favor one specific scenario. Despite
the great effort of observers in the last decades, interstellar magnetic fields (MFs) still represent an importantunknown in filament formation. Polarized thermal emission at sub-millimeter and far-infrared wavelengths frominterstellar dust grains is the most suitable technique to investigate the density-weighted MF-structure in the
ISM. Only very recently, the Planck satellite has completed the first all-sky maps of dust polarization at 850
microns, allowing us to probe the correlation between the MF geometry and the filamentary density structurewith unprecedented statistics. In this talk I will present results on the relative orientation between the MF andthe density structure in the ISM, from the diffuse medium to MCs. The probe of the MF properties in MCs andin their diffuse surroundings is crucial to understand the initial conditions relevant for the formation of starforming filaments. In the Planck data, filaments seen in total intensity are observed statistically aligned with the
MF orientation in the diffuse ISM, while they become statistically perpendicular to the MF in denser regions in
MCs. I will discuss the implications of this correlation in the context of filament formation.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 11:50
Name: Simon Glover
Organisation: Institute for Theoretical Astrophysics - University of Heidelberg
Title: Hunting for observational signatures of molecular cloud formation
Abstract:
In order to better understand how molecular clouds form in the galactic interstellar medium, we would like tobe able to map the structure and kinematics of the gas flows responsible for forming them. However, it is not
immediately obvious which observational tracers we should use in order to do this. CO, the workhorse moleculefor studies of molecular clouds, is a poor choice, as it traces only relatively dense gas in those portions of theclouds that have already assembled and tells us little about the surrounding gas flows. Numerical simulations

13

suggest that these flows are composed of a mixture of HI and CO-dark H2 and allow us to study the propertiesof the emission that we expect to detect from them. In this talk, I will present results from a series of recent
numerical simulations of cloud assembly and will discuss what these simulations can teach us about the best
observational strategies to use when searching for signatures of cloud formation.
-------------------------------------------------------------------------------------------------------------------------------------- ------------Time of talk: Monday 12:10
Name: Ana Duarte Cabral
Organisation: University of Exeter
Title: Observing simulations: Molecular clouds and their journey in the Galaxy
Abstract:
Stars form within molecular clouds, which are formed as a result of the interchange and evolution of gas througha wide range of densities and scales. Therefore, to understand the global processes that lead to star formation,
it is crucial to understand the hierarchical organisation of the molecular component of the interstellar medium.
However, defining and extracting clouds is not an easy task: molecular clouds are not a discrete well-defined
entity - instead, they are part of a continuum of gas that travels through the galaxy, and often a mix of different
fractions of atomic and molecular gas components, and different abundances of molecular species such as CO.
Moreover, Milky Way studies suffer from yet another issue: a severe line of sight confusion that complicates theidentification of “real” individual GMCs. Here I will present our recent work trying to grasp some of these issues,by studying the population of GMCs from a simulation of a portion of a spiral galaxy. We have used a newalgorithm (SCIMES) to extract GMCs from both the physical 3-dimensional space, and from an observer’s
perspective on CO emission datacubes. I will present the results from comparing the properties of clouds
retrieved from the different extractions, as a means to understand the biases inherited from the perspective,
resolution and tracer used. I will also explore how different galactic environments can affect GMC properties,
namely by following the clouds as they travel from the shear-dominated inter-arm regions into and throughspiral arms.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 12:30
Name: Eric Keto
Organisation: Harvard-Smithsonian Center for Astrophysics
Title: A simple description of the energy budget in molecular clouds and their atomic envelopes
Abstract:
The energy budget of molecular clouds and their atomic envelopes is one of radiative equilibrium. For use in 3D
numerical hydrodynamics, we develop the simplest possible description of this equilibrium leading to gas
temperature. I will describe the model for gas and dust heating and cooling and how the model is benchmarked
with observations. The chemical model for the abundances of the major gas coolants, CO, C+, and O, is checkedby comparison with spectral line observations made with the Herschel satellite and with the IRAM 30m. The
model for the dust is checked against multifrequency observations of submm dust emission also made with
Herschel. This model for radiative equilibrium and the gas temperature has recently been incorporated into a
3D SPH code with applications for star formation (Bate and Keto, MNRAS 2015) and the first results, comparison
with other more complex models, are described.

14

Time of talk: Monday 12:50
Name: Volker Ossenkopf-Okada
Organisation: University of Cologne
Title: Column density PDFs as a diagnostic tool
Abstract:
The most simple statistics to characterize the structure seen in maps of interstellar clouds is given by counting
the observed intensity or column density values. The resulting probability distribution functions (PDFs) have acharacteristic shape determined by the physical processes driving structure formation in the clouds.
Measuring these functions is, however, not trivial due to observational limitations. Careful corrections caneliminate the effects of observational noise and line-of-sight contamination. The selection of the map edges isalready critical and it turns out that ALMA observations are basically unusable to obtain a reliable statistics.
Column density PDFs from dust cover a much larger dynamic range than any molecular-line based PDF, but only
the latter ones allow to fully avoid line-of-sight confusion.
The major part of the PDFs, usually described by a log-normal function, is often attributed to turbulence, but infact, the statistics is often insufficient for this assignment. The power-law tail commonly found in the PDFs iscaused by the gravitationally driven collapse of filaments and clumps. Different collapse geometries lead todifferent exponents that are directly measurable. Infrared dark clouds exhibit the same PDF features as more
nearby, actively star-forming clouds, proving the same nature of both types of clouds. For a small number ofclouds we find, moreover, clear signatures of the phase transitions between atomic and molecular hydrogenand for the impact of radiative feedback on the column density statistics.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 14:40
Name: Seamus Clarke
Organisation: Cardiff University
Title: Fragmentation of accreting filaments
Abstract:
We use smoothed particle hydrodynamic simulations to investigate the growth of perturbations in infinitely
long, initially sub-critical but accreting filaments. The growth of these perturbations leads to filament
fragmentation and the formation of cores. Most previous work on this subject has been confined to the growthand fragmentation of non-accreting equilibrium filaments and has found that there exists a preferential
fragmentation length scale which is roughly 4 times the filament's diameter. Our results show a more
complicated dispersion relation with a series of peaks linking perturbation wavelength and growth rate. These
are due to gravo-acoustic oscillations along the longitudinal axis during the sub-critical phase of growth, when
the filament is far from equilibrium. The positions of the peaks in growth rate have a strong dependence on boththe mass accretion rate onto the filament and the temperature of the gas. When seeded with a multi-wavelengthdensity power spectrum there exists a clear preferred core separation equal to the largest peak in the dispersion
relation. Our results allow observers to estimate a minimum age for a filament which is breaking up into regularly
spaced fragments, as well as a maximum accretion rate. We apply the model to recent observations by Tafalla& Hacar (2015) of fragmenting sub-filaments in Taurus and find accretion rates consistent with those estimatedby Palmeirim et al. (2013).

15

Time of talk: Monday 15:00
Name: Jouni Kainulainen
Organisation: Max Planck Institute for Astronomy
Title: Fragmentation of the Integral Shaped Filament in Orion A as viewed by ALMA
Abstract:
High line-mass filaments are birthplaces of high-mass stars and star clusters and thus important for Galactic scalestar formation. However, description of their fragmentation and collapse process is yet fundamentally lacking.
We have performed the most sensitive fragmentation study of a high line-mass filament to date: we have used
ALMA 3 mm continuum data to characterize fragmentation of the Integral Shaped Filament in Orion A down to
1 000 AU scales. The dense cores detected in the data indicate a two-mode fragmentation picture: periodic
fragmentation into groups of cores and further fragmentation within those groups. Any current gravitational
fragmentation models do not predict such pattern; we discuss possible processes leading to it. We also compare
the spatial distribution of dense cores to protostars and stars with disks. The protostars are grouped similarly
with the dense cores, while stars with disks have clearly different distribution. This indicates that the maternalgrouping of dense cores is retained over the protostar lifetime, but not over the lifetime of stars with disks. Thisin turn suggests that the distribution of stars loses the memory of its origin rapidly after stars decouple from gas.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 15:20
Name: Kate Pattle
Organisation: University of Central Lancashire
Title: First results of the JCMT BISTRO survey: The magnetic field of Orion A
Abstract:
We present the first results from the BISTRO (B-Fields in Star-Forming Region Observations) Survey. BISTRO isusing the newly-commissioned POL-2 polarimeter on the JCMT to map the submillimetre emission from highcolumn-density regions of nearby star-forming clouds to unprecedented depth in polarised light. BISTRO is
producing a large and homogeneous polarisation data set, mapping the magnetic fields in star-forming regions
on scales as small as 1000 AU, allowing investigation of some of the most important questions in star formation,
particularly the relative importance of magnetic fields and turbulence to the energy balance and evolution ofstar-forming regions. As a demonstration of the science which BISTRO will achieve, we present early results ofobservations of the Orion A molecular cloud. We present maps of the magnetic field structure of the OMC 1
star-forming region, along with estimates of magnetic field strengths determined through synthesis with carbon
monoxide data taken as part of the JCMT Gould Belt Survey using the Chandrasekhar-Fermi method. We showthat the field in the centre of the Orion BN-KL region shows an 'hourglass' morphology, with field lines runningapproximately perpendicular to the central filament. We discuss the consistency of these observations with therecently-proposed model of filament growth in which material is funnelled onto filaments along magnetic fieldlines, and discuss the interaction between the Orion BN-KL outflow and the local magnetic field. We further
show that the polarisation vectors around the Orion Bar are consistent with the Orion Bar being wrapped by ahelical magnetic field, and discuss the contribution of magnetic energy to the energy balance of both the Orion
BN-KL and Orion Bar regions.

16

Time of talk: Monday 15:40
Name: Huei-Ru Vivien Chen
Organisation: National Tsing Hua University
Title: Filamentary Accretion Flows in the IRDC M17 SWex
Abstract:
Although filamentary structures are ubiquitous in molecular clouds, basic observational constraints are needed
to clarify the role of filaments in the mass assembling process. We have observed with ALMA the N2H+ and HNCemission in the filamentary accretion flows in the remarkable IRDC complexes, M17 SWex, where a delayed
onset of massive star formation was reported in the two hubs at the convergence of multiple filaments of parsec
length. We derived the kinematics with the N2H+ emission and found the line widths are smaller than those ofammonia, suggesting a transonic nature of dense gas in the filaments. Slow infall motions are detected along
the filaments. Multiple velocity coherent substructures are present in both hubs, likely not yet reaching virial
equilibrium.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 16:50
Name: Jonathan Henshaw
Organisation: Liverpool John Moores University
Title: Seeding the Galactic Centre gas stream: initial conditions for the formation of Young Massive Clusters
Abstract:
The Central Molecular Zone of the Milky Way contains some of the most massive and dense molecular clouds
and star clusters in the Galaxy, offering an important window on star formation under extreme conditions. Starand cluster formation in this extreme environment may be closely linked to the orbital dynamics of the gas, thethree dimensional distribution of which has been subject to intense scrutiny for several decades. One of themost striking features of the CMZ, noted from the earliest studies, is the complex gas distribution in positionposition-velocity (PPV) space. In this contribution, I will present our new systematic approach to studying thekinematics of dense gas in the central 250pc of the Galaxy, demonstrating how this has helped to accurately
describe the {l,b,v} structure of the CMZ. I will demonstrate how this analysis can help to distinguish between
the three geometries commonly cited within the literature to describe the 3-D structure of the CMZ. Finally, I
will present the recent discovery of intriguing oscillatory patterns in the kinematic structure of the dense gas.
Perhaps an observational sign-post of gravitational instabilities within the gas, this has, if confirmed, significant
implications for understanding the formation of some of the most massive and dense molecular clouds within
the Galaxy and may represent the earliest phases in a directly observable (absolute) time sequence for starformation.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 17:10
Name: Joao Alves
Organisation: University of Vienna
Title: Blue Streams and local star formation
Abstract:
We construct a 3D map of the spatial density of OB stars within 500 pc from the Sun using the Hipparcos
catalogue and find three large-scale stream-like structures that allow a new view on the solar neighborhood.

17

The spatial coherence of these blue streams and the monotonic age sequence over hundreds of parsecs suggestthat they are made of young stars, similar to the young streams that are conspicuous in nearby spiral galaxies.
The three streams are 1) the Scorpius to Canis Majoris stream, covering 350 pc and 65 Myr of star formation
history, 2) the Vela stream, encompassing at least 150 pc and 25 Myr of star formation history, and 3) the Orion
stream, including not only the well-known Orion OB1abcd associations, but also a large previously unreported
foreground stellar group lying only 200 pc from the Sun. The well-known nearby star-forming low-mass clouds,
including the nearby T and R associations Lupus, Cha, Oph, CrA, Taurus, and various low-mass cometary clouds
in Vela and Orion, appear in this new view of the local neighborhood to be secondary star formation episodes
that most likely were triggered by the feedback from the massive stars in the streams.
We find no evidence of an elliptical structure such as the Gould Belt, a structure we suggest is a 2D projection
effect, and not a physical ring. We present Herschel data on Ophiuchus where we find that all protostars in
Ophiuchus (97%) can be readily associated with a particular source of feedback in the region and that the
Ophiuchus filaments (up to 20 pc long) are also formed by the feedback from massive stars, in contrast with thecurrently accepted filament formation scenario of colliding flows orthogonal to the filament axis. Finally, we do
not find N-PDFs to be log-normal, but power-laws.
-------------------------------------------------------------------------------------------------------------------------------------- ------------Time of talk: Monday 17:30
Name: Emily Drabek-Maunder
Organisation: Imperial College London
Title: The JCMT Gould Belt Survey: Understanding the influence of molecular outflows on Gould Belt clouds
Abstract:
Using James Clerk Maxwell Telescope (JCMT) Gould Belt Survey data from CO J=3-2 isotopologues, we present
a meta-analysis of the outflows and energetics of star-forming regions in several Gould Belt clouds. The majorityof the regions are strongly gravitationally bound. There is evidence that molecular outflows transport large
quantities of momentum and energy. Outflow energies are at least 20 per cent of the total turbulent kinetic
energies in all of the regions studied and greater than the turbulent energy in half of the regions. However, wefind no evidence that outflows increase levels of turbulence, and there is no correlation between the outflow
and turbulent energies. Even though outflows in some regions contribute significantly to maintaining turbulence
levels against dissipation, this relies on outflows efficiently coupling to bulk motions. Other mechanisms (e.g.
supernovae) must be the main drivers of turbulence in most if not all of these regions.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Monday 17:50
Name: Enrique Vazquez-Semadeni
Organisation: RyA-UNAM
Title: Core structure and evolution in globally collapsing molecular clouds
Abstract:
After a brief motivation for the scenario that molecular clouds are in a state of global and hierarchicalgravitational collapse, consisting of collapses within collapses, I will discuss the evolution and structure of clumps
and dense cores in numerical simulations of cloud formation within this scenario. The clumps exhibit a scaling
relation of the form sigma_v^2/R ~ Sigma, where sigma_v is the velocity dispersion, R is the cloud ""radius"",and Sigma is the column density. This relation is similar to that observed for GMCs and massive star-forming
clumps, suggesting that the global-collapse scenario correctly describes their internal structure. Concerning theevolution of dense cores, I will also discuss numerical simulations of the prestellar collapse of near-Jeans-mass

18

cores embedded in a multi-Jeans-mass initially uniform background medium. The evolution of these cores
closely traces the locus of both low- and high-mass observed dense core ensembles in an M_c/M_BE vs. M_cdiagram introduced by Lada et al. (2008), where M_c is the core mass and M_BE is the Bonnor-Ebert mass at
the mean density and temperature of the cores. The collapse proceeds in an outside-in fashion, which implies
that infall speed estimates based on blue-excess line profiles may underestimate the actual velocities arising in
the core.

19

20

Tuesday 23rd August

Protostellar Cores
Talk Abstracts

21

Time of talk: Tuesday 9:00
Name: Kengo Tomida
Organisation: Osaka University
Title: Theory review
Abstract:
In this talk I review recent progress in theoretical studies of formation and evolution of stars and disks incollapsing molecular cloud cores. I start from classical problems in the early phase of star and disk formation (i.e.
until early Class 1 phase), such as the angular momentum problem, the magnetic flux problem, the magnetic
braking catastrophe, the fragmentation crisis, driving of outflows, and so on. In particular, while the angularmomentum problem and the magnetic braking catastrophe are now reconciled qualitatively, but they still
remain as qualitative problems. Then I move to the later phase of star formation and discuss outstanding topics
such as the luminosity problem, episodic accretion, and regulation mechanisms of star formation efficiency inthe small scale in different mass regimes, among other things. Also, if time permits, I briefly review recent effortson theoretical modeling and synthetic observations that enable us to directly compare theories and observations
especially using ALMA. At the end I would like to summarize the remaining (and new) problems, (near) future
directions, and (quite personal) perspectives.
-------------------------------------------------------------------------------------------------------------------------------------- ------------Time of talk: Tuesday 9:40
Name: Anaëlle Maury
Organisation: CEA/Saclay
Title: Observational review
Abstract:
While the physical processes regulating the formation and evolution of star-forming cores are believed to largely
determine the properties of the resulting young stars, their study has been mostly limited to shallow- and lowresolution observations. The advent of Herschel and large (sub-)millimeter interferometers (ALMA, NOEMA)
recently allowed to over-come these limitations, and carry out detailed and/or statistical studies of the cores
physical structure and chemical composition, to finally unravel the complex interplay of processes at work toform stars from these cores. I will review recent observational results, showing how the combination of highangular resolution and unprecedented sensitivity allow to finely characterize critical properties such as theangular momentum content, infall rates, pristine disk properties and multiplicity fraction of the youngest starforming cores.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 10:20
Name: Vera Könyves
Organisation: CEA/Saclay
Title: A census and properties of dense cores and filaments in the Aquila and Orion B cloud complexes
Abstract:
One of the main scientific goals of the Herschel Gould Belt survey (http://gouldbelt-herschel.cea.fr) is toelucidate the physical mechanisms responsible for the formation and evolution of prestellar cores in molecular
clouds. Based on Herschel/SPIRE-PACS photometric data, we have recently identified a large sample of suchcores in the Aquila (Könyves et al. 2015) and Orion B (Könyves et al., in prep.) molecular clouds.

22Our Herschel observations also provide an unprecedented census of filaments in the nearby clouds and suggest
an intimate connection between these filaments and the formation process of prestellar cores.We will compareand contrast some properties of the dense cores in the Aquila and Orion B complexes, such as their distributionsin the filamentary background, masses, lifetimes, and formation thresholds.
In summary, our Herschel findings support a filamentary paradigm for the early stages of star formation, where
the cores result primarily from the gravitational fragmentation of marginally supercritical filaments (cf. André etal. 2014, PPVI).
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 10:40
Name: Alana Rivera-Ingraham
Organisation: ESA
Title: Extreme Star Formation in the Galaxy: The Herschel View
Abstract:
The Herschel Space Observatory has provided extensive datasets of unprecedented quality and coverage. The
Archive covers regions in a wide range of physical and star-forming conditions across the Galaxy. Here we
introduce the latest results from an ongoing large-scale project focused on investigating the processes driving
star formation in the most extreme conditions. Compact sources and filamentary structures have been identified
and extracted from Herschel maps targeting the most active and densest regions of the Galactic Plane,comprising vigorous, high-mass star and cluster formation. Each structure was characterised according to its
physical and environmental properties, ongoing star formation and evolutionary state. The star-forming
conditions of these fields have been compared with those derived from the most diffuse, high-galactic latitude
fields with none or weak star forming events. Our extensive study provides new evidence in favour of the criticalrole of external and environmental factors in the overall star formation process, and how these factors
contribute to explaining the radically different star formation events in our Galaxy, from isolated low-mass starformation to massive clusters. This evidence will be summarised and discussed in context with theoreticalmodels of cloud evolution.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 11:50
Name: Isabelle Ristorcelli
Organisation: IRAP/CNRS-UPS Toulouse
Title: A statistical analysis of polarized dust emission in the environment of Planck Galactic cold clumps
Abstract:
Magnetic fields are considered one of the key physical agents that regulate star formation, but their actual rolein the formation and evolution of dense cores remains an open question. Polarized dust continuum emission isparticularly well-suited to probe the magnetic field structure in the dense, cold interstellar medium. Suchobservations also provide tight constraints on the efficiency of dust alignment along magnetic field lines, which
are needed to properly infer the magnetic field properties from observations. With the Planck all-sky survey of
dust submillimetre emission in intensity and polarization, we can investigate intermediate spatial scales in thehierarchy of star formation, between global molecular cloud measurements and studies of individual prestellar
cores. Planck further enables a statistical analysis of the polarization properties of clumps. We have recently
built the first all-sky catalogue of Galactic Cold Clumps (PGCC, Planck collaboration XXVIII 2015), a fraction ofwhich we have studied in detail with our Herschel Key Programme ‘Galactic Cold Cores’. The sources cover abroad range in physical properties and correspond to different evolutionary stages in the star formation process,23

from quiescent starless clumps and nearby cores to young protostellar objects. I will present new results from
our analysis of the polarized 353GHz Planck data for the PGCC sources. In particular, we have studied thevariation of the polarization fraction and angle, and the relative orientation between the B-field and the clump
elongations. We have also analysed the magnetic field morphology and compared it to structures (filaments,
striations) traced at higher resolution with Herschel in the environment of PGCC sources, searching forevolutionary signatures. Finally, I will present a comparison of our results with predictions from MHD simulations
that include radiative transfer and the dust radiative torque alignment mechanism.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 12:10
Name: Jennifer Hatchell
Organisation: University of Exeter
Title: Taking the temperature of local star-forming clouds with the JCMT Gould Belt survey
Abstract:
Radiative heating by recently-formed (or forming) stars potentially provides a regulatory mechanism for starformation, reducing fragmentation and increasing protostellar masses. I will report on work carried out by the
JCMT Gould Belt survey team on the contribution that SCUBA-2 data makes to measuring dust temperatures, on
its own and in combination with Herschel measurements.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 12:30
Name: Sarah Sadavoy
Organisation: Max Planck Institute for Astronomy
Title: Dust Emissivity in OMC 2/3: Linking the Diffuse Cloud to the Dense Cores
Abstract:
Planck observations have found relatively uniform values for the dust emissivity index of beta ~ 1.8 for diffuse
cloud material. Nevertheless, stars form within smaller-scale, denser environments where the dust grains are
expected to grow in size, form icy mantles, and subsequently have distinct dust emissivities compared to the
diffuse cloud. To explore this expected dust grain evolution, we combined Herschel observations with longwavelength 2 mm data across a ~ 2 pc long, continuous section of OMC 2/3 at 15000 AU (0.08 pc) resolution. We
determine beta and reconstruct simultaneously the filtered-out large-scale emission at 2 mm in thisanalysis. We find that beta ~ 1.7-1.8 provides the best fit across most of OMC 2/3 with only one protostellar
core showing significantly lower values of beta (~1.4). The consistency in beta between the cloud-scale Planck
data and our core-scale analysis for OMC 2/3 supports the common assumption of fixed beta indices usedubiquitously in the conversion of (sub)millimeter emission to mass in dense star forming regions. If thisconsistency is demonstrated in other clouds, then significant changes to dust grain properties may only beapparent on smaller (sub core) scales.

24

Time of talk: Tuesday 12:50
Name: Christopher Wright
Organisation: UNSW Canberra
Title: Magnetic fields via thermal infrared polarimetric imaging
Abstract:
Aligned dust grains within a magnetic field can induce polarization of thermal infrared radiation via emission,
absorption or both. The position angle of polarization is directly related to the magnetic field projected on to
the plane-of-the-sky. We will present new sub-arcsecond polarimetric imaging observations of embedded Young
Stellar Objects made with the CanariCam mid-IR camera/spectrometer on the 10.4 m Gran Telescopio Canarias.
By obtaining images across the 10 micron silicate band we can separate emissive and absorptive components ofpolarization and thus obtain two magnetic field directions, i.e. those within 'warm' and 'cold' regions of thetarget. For sources which are also extended we can then obtain a 3-d picture of the magnetic field.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 14:40
Name: Benoît Commerçon
Organisation: CRAL ENS Lyon
Title: Outflows and disks formation in massive cores collapse
Abstract:
Discs and outflows are observational features of star formation. While discs and outflows formation is becoming
increasingly constrained thanks to radiation magnetohydrodynamics models and observations in the context of
low-mass star formation, it is not the case for massive star formation. I will present results of massive magnetized
dense core collapse simulations including radiative feedback and ambipolar diffusion. We use the adaptivemesh-refinement code RAMSES (Teyssier 2002) which includes resistive MHD (Fromang et al. 2006, Masson etal. 2012) and radiative transfer (Commerçon et al. 2011, 2014). I will show how magnetic fields and radiative
feedback work together to launch outflows. I will study the formation and properties (early evolution andfragmentation) of the disc around the massive protostars, comforting the standard accretion-discs scenario in
the context of magnetised core collapse. Last I will also highlight the limits of ideal MHD with respect to magnetic
flux redistribution and outflow formation.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 15:00
Name: Yusuke Aso
Organisation: The University of Tokyo
Title: ALMA observations of Keplerian disks around protostars
Abstract:
Keplerian disks around young stars play essential roles in star and planet formation. Even though disks around T
Tauri stars have been studied well in the last two decades, the disk formation process prior to T Tauri phase isstill not well understood. This is because observations of disks around embedded protostars have been limited.
Such a situation, however, has been undergoing a dramatic transformation in the ALMA are.
To understand the disk formation around protostars in detail, we have been observationally studying 8
protostars (6 Class 0 and 2 Class I) with ALMA in mainly C18O (J=2-1) line and 1.3 mm continuum emissions at

25

sub-arcsec resolutions. All the sources show velocity gradients in C18O and detailed analyses using PV diagrams
revealed that 4 of them show Keplerian rotation, which is clearly distinguished from rotation of the envelopes.
Class 0 protostars tend to have less detectable disks, with lower specific angular momenta. It would be,therefore, suggested that our series of ALMA observations witness disk formation and growth during theprotostellar evolution although the results are not statistically significant yet. Dynamical stellar masses
estimated from the identified Keplerian rotation are compared with infall motions in their envelopes, findingthat some of the infall velocities are significantly slower than the free-fall velocities yielded by their dynamicalstellar masses.
The continuum visibility of L1527 IRS, which has an edge-on disk, is fitted by modified disk models without any
annulus averaging. This analysis is particularly important for non-axisymmetric structures, such as a disk. The
best model suggests that the density of dust is discontinuously enhanced at the boundary between the disk andthe envelope. Additionally, the scale height of the disk can be explained by hydrostatic equilibrium. These results
clearly demonstrate that ALMA observations can not only search for but also characterize in detail disks aroundprotostars.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 15:20
Name: Benjamin Lewis
Organisation: University of Exeter
Title: Shaken and stirred - the role of turbulence, magnetism and radiation in the formation of protostars.
Abstract:
Expanding on Lewis, et al (2015) and (2016, submitted), which considered only an ideal MHD simulations of thecollapse of molecular cloud cores without turbulence, we now use radiation magnetohydrodynamical
calculations to explore how the physics of turbulence, magnetism and radiation influence the formation of
protostars. We find that the gravitational collapse proceeds in a very different manner in cores with transonicturbulence compared to those with subsonic turbulence across a variety of field geometries and structures.
Transonic (i.e. ~ Mach 1) cores are highly disrupted by the turbulent motion which also suppresses the formationof bipolar jets from the first hydrostatic core. Cores with subsonic turbulence still contain a jet, albeit without
the symmetry previously seen in non-turbulent calculations and, depending on the magnetic field strength, form
pseudo-discs. The inclusion of radiative transfer into the calculations promotes the formation of large discs,
compared to the very small and dense discs produced by the MHD only calculations.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 15:40
Name: Neil Vaytet
Organisation: Niels Bohr Institute, University of Copenhagen
Title: A grid of 1D low-mass star formation collapse models: not all dense clouds form first Larson cores
Abstract:
Stars form within large turbulent molecular clouds from density fluctuations which become gravitationallyunstable. Numerical simulations of star formation are becoming ever more sophisticated, incorporating new
physical processes in increasingly realistic setups. These models are being compared to the latest observations
through state-of-the-art synthetic renderings that can identify the different chemical species present in the
protostellar systems. The chemical evolution of the interstellar and protostellar matter is a very active field of
research, with more and more chemical databases and reaction solvers becoming available online to thecommunity.

26

Time of talk: Tuesday 16:50
Name: Yusuke Tsukamoto
Organisation: RIKEN
Title: Bimodality of Circumstellar Disk Evolution Induced by the Hall Current
Abstract:
We investigate the effect of the Hall current term on the formation of the circumstellar disk using threedimensional simulations. In our simulations, all non-ideal effects, as well as the radiation transfer, areconsidered. We found that the size of the disk is significantly affected by a simple difference in the inherent
properties of the prestellar core, namely whether the rotation vector and the magnetic field are parallel or antiparallel. In the former case, only a very small disk (\lt 1 {AU}) is formed. On the other hand, in the latter case, amassive and large (\gt 20 {AU}) disk is formed in the early phase of protostar formation. Since the parallel andanti-parallel properties do not readily change, we expect that the parallel and anti-parallel properties are also
important in the subsequent disk evolution and the difference between the two cases is maintained orenhanced. This result suggests that the disk size distribution of the Class 0 young stellar objects is bimodal. Thus,
the disk evolution can be categorized into two cases and we may call the parallel and anti-parallel systems Orthodisk and Para-disk, respectively. We also show that counter-rotating envelopes against the disk rotation appear
with a size of ≳ 200 {AU}. We predict that the counter-rotating envelope will be found in the future observations.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 17:10
Name: Oliver Lomax
Organisation: Cardiff University
Title: Core fragmentation and protostellar multiplicity
Abstract:
Using an ensemble SPH simulations, we follow the evolution of prestellar cores as they collapse and fragment
into protostars. The initial conditions for these simulations are constructed to match the observed properties of
the cores in Ophiuchus. The protostars that form match the statistics of observed young protostars (IMF andmultiplicity statistics, including triples, quadruples, quintuples and sextuples) but only if (i) radiative feedback
from protostars is episodic, and (ii) the turbulent velocity field has a significant solenoidal component. A majorityof protostars are attended by significant discs, but in multiple systems these discs are often poorly aligned with
one another and/or the binary orbit, reflecting the stochastic nature of the accretion flows that feed material
into the centre of a core. We also present synthetic spectra and images of multiple systems embedded inprotostellar cores. These are calculated using a new Smoothed Particle Monte Carlo Radiative Transfer
algorithm.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 17:30
Name: Joana Oliveira
Organisation: Keele University
Title: Herschel Spectroscopy of Massive Young Stellar Objects in the Magellanic Clouds
Abstract:
As the nearest gas-rich galaxies, the Large and Small Magellanic Clouds (LMC and SMC) offer the exciting
opportunity to bridge the gap between star formation processes on large galaxy-wide scales and on the small

27

scales of individual Young Stellar Objects (YSOs). These metal-deficient galaxies also provide an invaluablewindow into the star formation process at low metallicity, a region in the parameter space that remains relatively
unexplored. I present the results of spectroscopic observations obtained with PACS and SPIRE/FTS onboard the
Herschel Space Observatory. The sample of massive SMC and LMC YSOs is well characterised at near- and midIR wavelengths, and includes both deeply embedded sources and compact HII regions. The strengths of key gasphase cooling species ([OI], [CII], H2O, CO, OH) are measured as probes of the physical conditions of the gas
surrounding the YSOs. This analysis directly probes the potential metallicity effect, since it quantifies the relative
luminosities of the species that promote envelope cooling and thus constrain the cooling budget of the YSO
envelopes. The results indicate that while [OI], [CII] and CO are easily and widely detected, H2O and OH may be
weak or absent in most YSOs. When compared with massive Galactic YSOs, the Magellanic YSOs clearly exhibit
higher photoelectric efficiency (measured by the ratio of line emission to total IR flux), while showing similar[OI]/[CII] ratios; in terms of standard PDR models this suggests a lower G_0/n ratio. The CO ladder is used toconstrain the density and temperature of the emitting gas. The spatial extension and morphology of the main
emission lines is used to explore the interplay and feedback of the massive YSOs with their environments. I willplace such results in context by comparing SMC, LMC and Galactic samples, in order to constrain potential
metallicity effects on the star formation process.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Tuesday 17:50
Name: Joseph Mottram
Organisation: Max Planck Institute for Astronomy
Title: Fragmentation and disk formation in high-mass star formation
Abstract:
How do the composition and kinematics of massive star forming environments affect the properties of the highmass protostars that are forming in them? How is the degree of fragmentation and mass on disk-like scales
related to the larger reservoir of dust and gas that they reside in? Are the 10^-4 Msol/yr and higher massaccretion rates and/or flattened envelope structures required by many current theories to form the most
massive stars seen in real systems? Does feedback have more of an impact on large or small scales and what is
the size (and shape) of the mass reservoir systems forming massive stars? These are all key questions todeveloping a full, comprehensive and prescriptive theory of how the most massive stars form. What is more,
answering them requires multi-scale observations of both the continuum and molecular lines. I will present early
results from the CORE NOEMA large program, which is designed to answer such questions by combining
observations with multiple PdBI configurations and the IRAM 30m of 20 high-mass star forming regions with L>
10^4 Lsol. As such we have one of the largest datasets to date of high mass star forming regions with sensitivity
to emission on spatial scales from ~0.4 pc to <1000 AU, ideal for tackling these fundamental questions.

28

Wednesday 24th August

Splinter Sessions

29

Early Career Researchers Session (Alumni Auditorium, The Forum)
Organisers: Chris Brunt and Tim HarriesThis session is devoted to talks by early career researchers whose abstract submissions were highly ranked by
the SOC.
09:00

Sam Geen (CEA Saclay)
Feedback in molecular clouds

09:15

Jan Orkisz (IRAM/LERMA)
Turbulence versus star formation efficiency in Orion B

09:30

Gwen Williams (University of Cardiff)
What can filament dynamics tell us about core formation?

09:45

Joseph Booker (University of Toledo)
HST Scattered Light Imaging of Orion Protostars: Do Outflows Halt Infall?

10:00

Bilal Ladjelate (CEA Saclay)
Star-formation in the Ophiuchus Molecular Cloud: Similarities and diversity

10:15

Coffee break

10:45

Josefa Grossschedl (University of Vienna)
Resolved maps of Star Formation Rate and Efficiency in Orion A

11:00

Steve Mairs (University of Victoria)
How Do Protostars Assemble Mass? A Sub-Millimetre (JCMT) Variability Survey of Deeply
Embedded Protostars

11:15

Dominika Boneberg (University of Cambridge)
The midplane conditions of protoplanetary discs

11:30

Julia Roquette (Universidade Federal de Minas Gerais)
Near-Infrared variability of disk-bearing stars in Cygnus OB230

Planet Formation Imager Session (Forum Seminar Room 4)
Organiser: Stefan Kraus
Among the most fascinating and hotly-debated areas in contemporary astrophysics are the means by whichplanetary systems are assembled from the large rotating disks of gas and dust which attend a stellar birth.
Although important work is being done both in theory and observation, a full understanding of the physics ofplanet formation can only be achieved by opening observational windows able to directly witness the process
in action. The key requirement is then to probe planet-forming systems at the natural spatial scales over whichmaterial is being assembled. By definition, this is the so-called Hill Sphere which delineates the region of
influence of a gravitating body within its surrounding environment. The Planet Formation Imager project has
crystallized around this challenging goal: to deliver resolved images of Hill-Sphere-sized structures withincandidate planet-hosting disks in the nearest star-forming regions. Solving the riddle of planetary formation has
profound and far-reaching implications beyond astronomy, for it helps inform our place in the universe andexpectations for life on other worlds.
09:00

John Monnier (University of Michigan)
Introduction to Planet Formation Imager Project

09:15

Stefan Kraus (University of Exeter)
The Science Vision for PFI

09:40

Mike Ireland (ANU)
A Baseline Design and Technical Roadmap for the PFI

10:05

Catherine Espaillat (University of Boston)
Detecting and characterising protoplanets with PFI

10:40

Coffee break

10:50

Johan Olofsson (MPIA)
Late stages of planetary system formation investigated with PFI

11:25

Sebastian Hoenig (University of Southampton)
Extragalactic science with PFI

31

Computational Star Formation Session (Forum Seminar Room 5)
Organiser: Simon Goodwin
The focus of this session is numerical simulations of star formation. There are talks on both numerical methods
and recent results. The last part of the session will be devoted to a discussion of future directions forcomputational star formation.
09:00

Daniel Seifried (University of Cologne)

09:15

Munan Gong (Princeton)

09:30

Rachel Spowage (University of Cardiff)

09:45

Rajika Kuruwita (ANU)

10:00

Claire Esau (University of Sheffield)

10:30

Coffee break

11:00

Duncan Forgan (University of St. Andrews)

11:20

Discussion: Where next for computation?

32

Ages and timescales of young stars (Forum Seminar Room 6)
Organiser: Cameron BellA predictive theory of the formation and evolution of stars and planets is one of the fundamental goals ofmodern astronomy, however our understanding hinges upon the ability to assign precise and reliable ages toyoung stars. These ages are crucial to constraining any potential theory by providing timescales with which to
study the time-dependent physical processes occurring in young stars.
This splinter session aims to bring together scientists in the star formation community to discuss recent
developments related to the ages of young stars, and how to combine these improved ages with ancillary data
to further our understanding of star cluster formation in general. We will also focus on second-order effects
such as the local environment in which these stars from.
09:00

Mark Pecaut (Rockhurst University)
Advances and limitations in determining the ages and timescales of young stars

09:30

Justyn Campbell-White (University of Kent)
Classifying HII regions using shape analysis of IR bubbles

09:50

Christine Koepferl (University of St. Andrews)
Insights from synthetic star-forming regions: star formation rates and dust properties

10:1010:15

Poster pop-up

10:1510:40

Coffee break

10:40

Rob Jeffries (Keele University)
Ages from lithium depletion in young stars

11:00

Mario Guarcello (INAF - Osservatorio Astronomico di Palermo)
Photoevaporation and close encounters: how the environment around Cygnus OB2 affects theevolution of protoplanetary disks

11:20

Sami Dib (Niels Bohr Institute)
Feedback-regulated star formation: dual constraints on the star formation efficiency and the age
spread of stars in clusters

11:40

Dirk Froebrich (University of Kent)
Photometric monitoring of nearby young clusters as a Citizen Science Project33

Measuring temperatures and densities in star forming regions (Forum
Seminar Room 10)
Organiser: Jenny Hatchell
Rationale: Star formation theories predict temperatures and densities for clouds, filaments and cores. Neither
temperature nor density is a direct observable. This session aims to bring together researchers interested in
extracting these physical properties from observations (e.g. continuum surveys or molecular lines) to discussuseful datasets and methodology (e.g. Bayesian model fitting, radiative transfer models).
09:0010:30

Short talks, each finishing with a summary slide showing the main result(s) and a 'wish list' - what the
speaker would like to be able to do with his/her method/data/region but doesn’t know how toachieve. Questions at this point will be limited to clarifications.

09:00

Jenny Hatchell (University of Exeter)
Introduction

09:10

Yao-Lun Yang (University of Texas)
Modeling the Structure of a Class 0 Protostar, BHR71, with 3-D Dust Radiative Transfer Simulations

09:25

Fernando Olguin Choupay (University of Leeds)
The physical properties of the prototypical MYSO GL 2591

09:40

Jared Keown (University of Victoria)
The Green Bank Ammonia Survey

09:55

Jorge Abreu-Vicente (MPIA Heidelberg)
Fourier-space combination of Planck and Herschel images

10:10

Nadia Murillo (Leiden University)
The role of temperature and gas heating in multiple stellar system formation

10:30

Coffee break

11:0012:00

2-minute presentations of ’wish lists’ from relevant main session talks (Joe Mottram, Katherine
Johnstone, Emily Drabek, Jan Forbrich, & Jenny Hatchell), followed by open discussion based on theissues raised.

34

Thursday 25th August

Young Clusters & Protostars
Talk Abstracts

35

Time of talk: Thursday 9:00
Name: Nick Wright
Organisation: Keele University
Title: Observational review
Abstract:
Over the last few decades our understanding of the properties of young stars and clusters has changed
dramatically thanks to many wide-field observations and surveys across the electromagnetic spectrum. Infrared,
X-ray and emission-line surveys have greatly increased our census of known pre-main-sequence stars, allowing
us to study their distribution and clustering, measure the initial mass function and multiplicity in different
environments, and study the ages and star formation histories of different regions. The rise in time domain
surveys has also improved our view of episodic accretion and variability in pre-main-sequence stars, while highresolution imaging has allowed us to study jets and outflows from such objects that exert feedback on theirsurroundings. In this talk I will review the current observational picture of the properties of young stars andclusters, with a particular focus on how wide-field surveys have contributed to our understanding of this criticalphase of stellar lives.
-------------------------------------------------------------------------------------------------------------------------------------- ------------Time of talk: Thursday 9:40
Name: Stella Offner
Organisation: UMass Amherst
Title: Theory review
Abstract:
Star formation is governed by the complex interplay of various physical forces, including turbulence, gravity andmagnetic fields. In addition, neighboring stars greatly influence each other and their natal cloud by injecting
energy into their surroundings (“feedback”). This interaction creates strong coupling between physical processes
acting over a broad range of scales. Numerical simulations play an essential role in investigating the complex,
nonlinear physics of star cluster formation. In this talk, I will summarize the current state-of-the-art in numericalsimulations. I will discuss how numerical results have shaped our understanding of star formation and how
different processes impact fundamental quantities like the stellar initial mass function, stellar multiplicity andstar formation efficiency.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 10:20
Name: Richard Parker
Organisation: Liverpool John Moores University
Title: The initial conditions of star formation from spatial and kinematic substructure
Abstract:
One of the largest uncertainties in star formation is the initial density and velocity structure of young (1 - 10Myr) star-forming regions, clusters and associations. Quantifying the initial or maximum density of a region is
crucial; a dense region will disrupt the orbits or destroy planetary systems and stellar binaries, andphotoevaporate or truncate protoplanetary discs through interactions with massive and low-mass stars.
However, the present-day density does not strongly constrain the initial density due to two-body relaxation,
which causes a region to rapidly expand and lowers the density by several orders of magnitude within a few

36

Myr. In this talk, I will show that a range of structural diagnostics can constrain both the initial density, and theinitial virial ratio of a star-forming region. I will finish by demonstrating the further constraints that Gaia andassociated ground-based surveys (e.g. GES) will place on this problem in the near future.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 10:40
Name: Isabelle Baraffe
Organisation: University of Exeter
Title: Consistent models of accretion history and multi-dimensional structure of accreting young stars.
Abstract:
I will present new results for pre-Main sequence and early brown dwarf evolutionary models accounting for theeffect of early accretion history. First, I will present self-consistent numerical simulations fully coupling numericalhydrodynamics models of collapsing prestellar cores and evolutionary models of the central protostar or protobrown dwarf. I will in particular analyse the main impact of consistent accretion history on Li depletion andpresent a new result regarding the effect of accretion on Li depletion. I will also present the first attempt todescribe the multi-dimensional structure of accreting young stars based on fully compressible time implicit
multi-dimensional hydrodynamics simulations. I will discuss the relevance of assumptions and treatments ofaccretion used in 1D stellar evolution codes.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 11:50
Name: Laura Venuti
Organisation: INAF - Osservatorio Astronomico di Palermo
Title: Variety of accretion regimes in the young open cluster NGC 2264
Abstract:
Pre-main sequence (PMS) stars are surrounded by disks throughout the first few Myr following their birth. The
star-disk interaction is governed by the magnetospheric accretion process. In this talk, we present the results ofan extensive u-band accretion survey of the 3 Myr-old open cluster NGC 2264. Performed at CFHT/MegaCam asa part of the CSI 2264 international campaign, the survey provided simultaneous UV+optical photometricmonitoring over two full weeks for about 750 young cluster members (of which about 45% have disks). We use
the diagnostics of the UV excess, measured over the reference flux level defined by non-accreting members, toinvestigate accretion properties over the stellar mass range 0.1-1.5 Mo, and infer evidence for a huge variety ofaccretion regimes within the cluster. While a definite correlation is observed between the average accretion
rate M_acc and stellar mass, a significant spread in M_acc values is detected at any given stellar mass. Little
contribution to this spread arises from M_acc variability, monitored here over week timescales. We explore anddiscuss the origin of this large intrinsic spread, which may be associated with a multiplicity of accretionmechanisms: unstable accretion regimes, characterized by short-lived, stochastic accretion bursts, are found to
be dominant at the largest M_acc; conversely, stable, funnel-flow accretion regimes, with a steady behavior
over many rotational cycles, are found at more moderate accretion rates. In addition, we find a connection
between accretion properties and spatial distribution of cluster members: strong accretors are assembled close
to the active star forming sites within the cloud, whereas milder accretors and disk-free objects distribute more
evenly across the region, possibly as a result of dynamical evolution from their birth sites. This suggests that an
intrinsic age/evolutionary spread across the cluster may also contribute to the observed spread in M_acc at any
given mass.

37

Time of talk: Thursday 12:10
Name: Alicia Aarnio
Organisation: University of Michigan
Title: Assessing Magnetospheric Accretion in Herbig Ae/Be Stars
Abstract:
In the last few years, large spectropolarimetric surveys have found low magnetic field detection rates in Herbig
Ae/Be stars. It has also been recently noted that magnetic field structure and strength dramatically change withincreasing stellar mass. These results are very suggestive that the mechanisms for accretion and outflow in
Herbig Ae/Be star+disk systems may differ from the magnetospheric accretion paradigm as envisaged for T Tauri
star+disk systems. We present the results of our high resolution optical spectroscopic campaign of ~60 Herbig
AeBe stars. Our survey includes multi-epoch observations; the timescales sampled range from high cadence(~minutes) to observations taken over several years, probing a wide range of kinematic processes. We find thatthe strength of variability increases with the cadence of the observations, and over all timescales sampled, thestrongest variability occurs within the blueshifted absorption components of the Balmer series lines. We see no
inverse P-Cygni profiles, traditionally indicative of ongoing accretion. We discuss the implications of these resultsin context of recent spectropolarimetric surveys for our understanding of how accretion is occurring in theseobjects, as well as ongoing radiative transfer modeling.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 12:30
Name: Carlo Felice Manara
Organisation: ESA/ESTEC
Title: Disk evolution in young clusters: accretion, winds, and dynamical properties of young stars and their disks
Abstract:
The evolution of protoplanetary disks in young stellar clusters is regulated by the interplay of various physicalprocesses, such as accretion and winds, and by the interactions with other stars in the cluster. Accretion andwinds are best studied spectroscopically. Instruments like the VLT/X-Shooter spectrograph allow us to observe
simultaneously the signatures of the accretion process, such as the UV-excess and the emission lines, together
with lines tracing winds and outflows, such as helium lines and forbidden lines. At the same time, such spectra
allow us to robustly derive the physical parameters of the central objects, such as their temperature and theirmass. These processes relate to the disk mass and size, which can nowadays be studied with ALMA. Finally, thecoming Gaia data releases will open the field to new studies of dynamical evolution of stars in young clusters bymeans of kinematical modelling.
I will report on the stellar, accretion, and wind properties derived with X-Shooter of the complete samples of
low-mass stars in the Lupus and Chamaeleon star forming regions, and discuss the dependence of stellar andaccretion parameters with the disk properties obtained with ALMA surveys in these regions. I will also show how
we can use Gaia data to study young clusters and the effect of interactions on the evolution of disks.

38

Time of talk: Thursday 12:50
Name: Philip Lucas
Organisation: University of Hertfordshire
Title: A population of eruptive variable protostars in VVV
Abstract:
We present the recent discovery of a substantial population of optically hidden eruptive variable protostars in
VISTA Variables in the Via Lactea survey (VVV). VVV was the first panoramic time domain survey of the Milky
Way in the near infrared. It ran from 2010-2015, observing a 560 sq deg area of the Galactic bulge and plane
between 50 and 70 times in the Ks filter. A wide variety of high amplitude infrared variables were detected(DeltaKs > 1 mag) but YSOs represent about half of the population. The YSOs have a variety of light curve types
but a substantial proportion can be described as photometric outbursts. Most of these "eruptive" variables
appear to be bona fide examples of episodic accretion, similar to the FUor and EXor phenomena. However, their
outburst durations and spectroscopic properties are a mix of the FUor and EXor types; those established types
are much rarer in the sample. We provisionally refer to these mixed sources as MNors, after the illuminating
source of McNeil's Nebula, V1647 Ori. Eruptive variability is at least an order of magnitude more common
amongst class I YSOs than in class II YSOs: we will present a first estimate of the incidence in class I YSOs. FinallyI describe the planned "VVVX" extension of VVV to the rest of the southern plane, which is currently at thesecond and final stage of the ESO public survey selection process.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 14:40
Name: Matthew Bate
Organisation: University of Exeter
Title: The dependence of stellar properties on metallicity
Abstract:
I will present the results of four radiation hydrodynamical calculations of star cluster formation that span
metallicities ranging from 1/100 to 3 times the solar value. The calculations treat both the thermodynamical
evolution of the low-density interstellar medium (including hydrogen and carbon chemistry), and radiationtransport which dominates temperatures near protostars. I will discuss the statistical properties of the stars andbrown dwarfs that are produced, including how the mass function, multiplicity, and properties of multiple
systems depend on the metallicity of the progenitor cloud.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 15:00
Name: Thomas Megeath
Organisation: University of Toledo
Title: Low Mass Star Formation in the Diverse Environments of Orion: Result from the Herschel Orion Protostar
SurveyAbstract:
Low mass stars from in a diverse range of environments, from isolated dark clouds to dense clusters in close
proximity to massive stars. How the low mass star formation process differs between these environments is notwell understood. We do know that within this range of environments, the densities of young low mass stars
varies by orders of magnitude, yet the initial mass function remains relatively invariant. Comparative studies of39

protostars in these environments are needed to assess how variation in gas density, turbulence and kinetic
temperature affect the fragmentation, collapse and accretion of gas and the formation of stars and disks. I will
overivew a survey of protostars in the Orion A & B molecular clouds with the Spitzer, Herschel, Hubble and Apex
telescopes, spanning 1.6 to 870 um, as well as follow-up observations in the near-IR and sub-millimeter. The
goals of these observations are to characterize multiplicity, infall, accretion, outflow, and disk formation in thediverse environments found in the Orion clouds. These observations find a decrease in the spacing of protostars
with increasing gas density, an increase of protostellar luminosity with increasing gas density, and an increasein the number of companions with increasing stellar density. I will discuss how these observations are leading
to a better understanding of the physical factors, both external and internal, that control the rate and efficiency
at which low mass stars form and ultimately determine their multiplicity and masses.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 15:20
Name: Jan Forbrich
Organisation: University of Vienna
Title: The Orion Radio All-Stars: new perspectives in stellar radio astronomy
Abstract:
The sensitivity upgrades of both the NRAO Very Large Array (VLA) and the NRAO Very Long Baseline Array (VLBA)
have begun to provide us with a much improved perspective on stellar centimeter radio emission, particularly
concerning young stellar objects (YSOs) and ultracool dwarfs. I will mainly present a deep VLA and VLBA radio
survey of the Orion Nebula Cluster (ONC), where we have found 556 compact radio sources, a sevenfold increaseover previous studies, and intricate detail on the radio emission of proplyds. We can now better disentangle
thermal and nonthermal radio emission by assessing spectral indices, polarization, variability, and brightness
temperatures (VLBA). With simultaneous radio-X-ray time domain information (Chandra) and VLBA precision
astrometry, this project is providing unpredented constraints on the magnetospheric activity of YSOs across awide mass range, new insights into the impact of the massive Trapezium stars on their environment, and new
astrometric constraints on the ONC itself. Additionally, I will present new VLBA results in ultracool dwarf
astrometry. More generally, and beyond providing a new perspective on stellar cm radio emission and physics,
this presentation will highlight how VLBI astrometry will allow us to extend the Gaia sample of YSOs and ultracool
dwarfs by including embedded objects, distant obscured sources in the Galactic plane, and faint ultracool dwarfs,
while providing important opportunities for astrometric cross-calibration with Gaia.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 15:40
Name: Nadia Murillo
Organisation: Leiden University
Title: Do siblings always form and evolve at the same time? Coevality of multiple protostellar systems with
Herschel
Abstract:
Multiplicity is common in field stars and protostars. While fragmentation is considered to be the mechanism of
formation, the question of when and how this occurs is still open. Previous studies towards pre-main sequencebinaries found pairs of non-coeval (different ages) components, with frequencies of 15 to 33%. Is this noncoevality present from the moment of formation or product of dynamical evolution? We address this question
by determining the relative evolutionary stages of the components in young embedded multiple protostellar
systems. Spectral energy distributions (SEDs) for known multiple protostellar systems in the Perseus star forming
region are constructed from literature data and Herschel PACS photometric maps. Inclination effects and the40surrounding envelope and outflows are considered in order to decouple source geometry from evolution. This
together with the shape and properties derived from the SED are used to accurately determine each system's
coevality. Synthetic SEDs are used to study the frequency of apparent non-coevality due to geometry. Effects ofunresolved multiple protostellar systems on SED shapes are also investigated. We find 33% of multiple
protostellar systems in our sample to be non-coeval, with higher order multiples showing a tendency to be noncoeval. Random pairing of synthetic SEDs suggest an apparent non-coevality frequency of 17%, however oursample does not show signs of strong geometric effects, hence the observed non-coevality is real. The
implications that the non-coevality frequency found in our work has on formation mechanisms and evolution
are examined.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 16:50
Name: Megan Reiter
Organisation: University of Michigan
Title: Powerful jets driven by intermediate-mass protostars in the Carina Nebula
Abstract:
We present new spectroscopy and Hubble Space Telescope imaging of protostellar jets driven by intermediatemass stars in the Carina Nebula. New, near-IR [Fe II] observations of these jets reveal dense gas that is selfshielded from Lyman continuum photons from nearby O-type stars, but is excited by non-ionizing FUV photons
that penetrate the ionization front within the jet. Each jet contains a substantial mass of dense, neutral gas thatis not seen in Halpha emission from these jets. In some cases, [Fe II] emission traces the jet inside its natal dust
pillar, connecting the larger Halpha outflow to the embedded IR source that drives it. New proper motion
measurements reveal tangential velocities similar to those typically measured in lower-luminosity sources (100200 km/s). Combining high jet densities and fast outflow speeds leads to mass-loss rate estimates an order ofmagnitude higher than those derived from the Halpha emission measure alone. Higher jet mass-loss rates
require higher accretion rates, implying that these jets are driven by intermediate-mass (~2-8 Msun) protostars.
For some sources, mid-IR luminosities of the driving sources are clearly consistent with intermediate-mass
protostars others remain deeply embedded and require long-wavelength, high-resolution images confirm theirluminosity. These outflows are all highly collimated, with opening angles of only a few degrees. With this newview of collimated jets from intermediate-mass protostars, we argue that these jets reflect essentially the sameoutflow phenomenon seen in low-mass protostars, but that the collimated atomic jet core and the material it
sweeps up is irradiated and rendered observable. Thus, the jets in Carina offer strong additional evidence thatstars up to ~8 Msun form by the same accretion mechanisms as low-mass stars.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 17:10
Name: Guido De Marchi
Organisation: European Space Agency
Title: The Tarantula of low-mass stars
Abstract:
We are studying the recent low-mass star formation in the Tarantula Nebula using the Hubble Tarantula Treasury
Project observations. Looking for stars with prominent Halpha excess emission (> 4 sigma, equivalent width >10A), we have identified more than 20,000 pre-main sequence (PMS) stars over an area of ~180 x 180 pc^2. We
are able to detect and study not only the youngest PMS objects, but also those approaching the main sequence,with ages older than ~10 Myr. This is so far the largest sample of individually resolved young low-mass stars.

41

We find that the distribution of PMS stars is considerably more diffuse than that of massive stars: while many
young PMS stars are often close to massive objects, a similarly high number of both young and older PMS objects
are clumped in regions with very few or no high-mass stars around. This implies that the conditions for theformation of low-mass stars are more lenient than those required by high-mass stars, and it might even suggestthat the relevant processes are quite different. This could have important implications for the concept of initial
mass function.
In the central regions, around the R136 cluster, we have already completed the analysis of the physicalproperties of both younger and older PMS stars. We confirm our previous findings on the dependence of themass accretion rate on the mass and age of the stars. We show that, in similar conditions of mass and age, in
the Tarantula Nebula the mass accretion rates are systematically higher than in the Milky Way, yet still lower
than those we measured in active star forming regions in the Small Magellanic Cloud. These findings appear toindicate that the metallicity of the environment may play a significant role in the mass accretion process.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 17:30
Name: Lee Hartmann
Organisation: University of Michigan
Title: Mass functions of star clusters and the upper mass stellar IMF
Abstract:
I will discuss numerical simulations which offer a simple, universal, and robust explanation of the star cluster(initial) mass function - gravitational focusing - with implications for the upper mass end of the stellar IMF.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Thursday 17:50
Name: Philippe André
Organisation: CEA Saclay
Title: The role of interstellar filaments in the origin of the stellar initial mass function
Abstract:
The origin of the stellar initial mass function (IMF) is one of the most debated issues in astrophysics. Two major
features of the IMF are 1) a fairly robust power-law slope at the high-mass end known since Salpeter (1955), and2) a broad peak below 1 Mo corresponding to a characteristic stellar mass scale. In recent years, the dominant
theoretical model proposed to account for these features has been the ""gravo-turbulent fragmentation""picture, whereby the properties of interstellar turbulence lead to the Salpeter power law and gravity sets thecharacteristic mass scale (Jeans mass). I will discuss modifications to this picture based on Herschel observationsof nearby molecular clouds. The Herschel results point to the key role of the quasi-universal filamentary
structure pervading the cold interstellar medium and support a scenario in which star formation occurs in two
main steps: First, large-scale compression of interstellar material in supersonic MHD flows generates a cobwebof ~ 0.1 pc-wide filaments in the ISM; second, the densest filaments fragment into prestellar cores above theline mass threshold for gravitational instability. In this observationally-driven scenario, the dense cores making
up the peak of the prestellar core mass function (CMF) - likely responsible for the characteristic IMF mass scale- result from gravitational fragmentation of filaments near the critical mass per unit length. The power-law tailof the CMF/IMF arises from the characteristic power spectrum of initial density fluctuations measured along the
Herschel filaments (Roy et al. 2015) and from the power-law distribution of masses per unit length observed forsupercritical filaments.

42

Friday 26th August

Discs
Talk Abstracts

43

Time of talk: Friday 9:00
Name: Catherine Espaillat
Organisation: Boston University
Title: Observational review
Abstract:
We know that most stars were once surrounded by protoplanetary disks. How these young disks evolve intoplanetary systems is a fundamental question in astronomy and observations of young pre-main sequence stars
may provide insights. In this talk, I will review the key constraints on theoretical models provided by observationsof the dust and gas in protoplanetary disks. I will discuss disk demographics and evolution as well as disk
structure, particularly those disks that contain holes or gaps which many researchers have posited are thefootprints of planets. Recent MIR and sub-mm imaging work will be discussed as well as remaining questions in
the field of protoplanetary disks.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 9:40
Name: Richard Alexander
Organisation: University of Leicester
Title: Theory review
Abstract:
In this talk I will review our understanding of protoplanetary discs. These discs are of considerable interest, as
they are both the primary means of driving protostellar accretion, and also the sites of planet formation. I will
briefly discuss disc formation and structure, and then look in detail at the various physical processes - angularmomentum transport in the disc, and mass and angular momentum loss in winds - which drive disc evolution.
This is a rapidly evolving field, so I will attempt to highlight key recent developments, as well as giving a criticalassessment of where the field currently stands. I will conclude by discussing future directions for our study ofdisc evolution, and the key questions we wish to answer in the coming years.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 10:20
Name: Tim Naylor
Organisation: University of Exeter
Title: A Dynamic Colour-Magnitude Diagram for the Orion Nebula Cluster
Abstract:
We have undertaken time-series multi-colour photometry of the Orion Nebula Cluster over seven nights, withsimultaneous multi-fibre spectroscopy. This allows us to construct "movies" of how the positions of stars incolour-magnitude space change with time, and use the spectroscopy to analyse the physical mechanisms driving
those changes. Whilst many stars remain largely static in position, some classical T Tauri stars show remarkable
peregrinations around the colour-magnitude space. Some changes are clearly due to changes in dust
obscuration, though there is evidence for grain growth in the extincting material. The degree of variability isclearly correlated with position in colour-magnitude space with the more variable stars lying below the majorityof the pre-main-sequence. As these are the classical T Tauri stars this leads to the remarkable conclusion thatin a colour magnitude diagram the heavily accreting stars classical T Tauri stars appear to be older than the disc-44

less weak-lined T Tauri stars. The simultaneous spectroscopy allows us to show that this is purely an effect of
the accretion luminosity.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 10:40
Name: Kenny Wood
Organisation: University of St Andrews
Title: A Model for (Quasi-) Periodic Multi-wavelength Photometric Variability in Young Stellar Objects
Abstract:
We present radiation transfer models of rotating young stellar objects (YSOs) with hotspots in theiratmospheres, inner disk warps and other 3-D effects in the nearby circumstellar environment. Our models are
based on the geometry expected from the magneto-accretion theory, where material moving inward in the disk
flows along magnetic field lines to the star and creates stellar hotspots upon impact. Due to rotation of the starand magnetosphere, the disk is variably illuminated. We compare our model light curves to data from the Spitzer
YSOVAR project to determine if these processes can explain the variability observed at optical and mid-infrared
wavelengths in young stars. We focus on those variables exhibiting ``dipper"" behavior that may be periodic,
quasi-periodic, or aperiodic. We find that the stellar hotspot size and temperature affects the optical and nearinfrared light curves, while the shape and vertical extent of the inner disk warp affects the mid-IR light curve
variations. Clumpy disk distributions with non-uniform fractal density structure produce more stochastic light
curves. We conclude that the magneto-accretion theory is consistent with certain aspects of the multiwavelength photometric variability exhibited by low-mass YSOs. More detailed modeling of individual sources
can be used to better determine the stellar hotspot and inner disk geometries of particular sources.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 11:50
Name: Gilles Chabrier
Organisation: University of Exeter & ENS Lyon
Title: Formation of proto-stellar and proto-planetary disks in star formation: the key roles of different physicalmechanisms
Abstract:
Protostar or protoplanetary disks are the link between the collapse of prestellar star-forming clumps at large
scales, and the formation of planet embryos at small scales. Understanding the magnetic, thermal and stability
properties of these disks, as well as the key problem of angular momentum transport during the core collapse,
are thus mandatory to have a reliable description of protostellar/protoplanetary disks. In this talk, I will present
calculations of disk formation that include the most complete relevant physics: non-ideal MHD, turbulence, nonequilibrium chemistry. The output of these calculations, disk properties and outflow signatures, will becompared with recent observations, allowing us to better understand the genesis and the nature of disks.

45

Time of talk: Friday 12:10
Name: Alvaro Ribas
Organisation: Boston University
Title: Protoplanetary disk lifetimes in nearby star-forming regions
Abstract:
The timescales and relevant parameters for protoplanetary disk evolution are crucial to fully understand planet
formation, but a consistent view of this phenomenon has remained elusive given its complexity and limited
sample sizes. In this contribution, I will present the most complete study of disk evolution up to date, performed
with a sample of more than 2300 YSOs in 22 nearby (<500 pc) star-forming regions and associations. The
unprecedented size of the sample and homogeneous treatments applied allowed us not only to derive the mostprecise measurement of the characteristic disk lifetime so far but also to statistically confirm an importantdependence of disk lifetimes with stellar mass. Such a dependence could even lead to differences in thearchitectures of planetary systems around low-mass and high-mass stars. Finally, I will describe our current
efforts on expanding these results with a more detailed subsample and advanced SED modeling techniques.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 12:30
Name: Melissa McClure
Organisation: European Southern Observatory
Title: T Tauri disk gas masses measured from hydrogen deuteride
Abstract:
The total gas mass of a protoplanetary disk is a fundamental, but poorly determined, quantity. A new technique(Bergin et al. 2013) has been demonstrated to assess directly the bulk molecular gas reservoir of molecularhydrogen using the HD J=1-0 line at 112 microns. In this work we present a small survey of T Tauri disk
observations of the HD line. Line emission is detected in two cases at >3 sigma significance. Using detailed disk
structure models, including the effect of UV gas heating, we determine the amount of gas required to fit the HD
line and the amount of dust required to fit the observed disk spectral energy distributions. For both disks, theamount of gas required is more than the MMSN value, and the gas/dust ratio is at least a factor of two lower
than that of the ISM. We discuss the implication of this result for these disks' carbon chemistry and the disk massprobability distribution.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 12:50
Name: Stefan Kraus
Organisation: University of Exeter
Title: Resolving the disc structure of FU Orionis stars
Abstract:
During their formation phase stars gain most of their mass in violent episodic accretion events, such as observedin FU Orionis stars. In this talk I will report on VLTI interferometric observations that allows us study the disk
structure around these objects on sub-AU scales.

46

Time of talk: Friday 14:40
Name: Katharine Johnston
Organisation: University of Leeds
Title: A Keplerian-like disc around the forming O-type star AFGL 4176
Abstract:
I will present our ALMA line and continuum observations at 1.2mm with ~0.3" resolution that uncover a
Keplerian-like disc around the forming O-type star AFGL 4176. The first-moment maps, pixel-to-pixel line
modelling, and position-velocity diagrams of the CH3CN J = 13–12 K-line emission all show a velocity gradientalong the major axis of the source, coupled with an increase in velocity at small radii, consistent with Keplerianlike rotation. I will also present APEX 12CO observations that show a large-scale outflow from AFGL4176
perpendicular to the major axis of mm1, supporting the disc interpretation. Finally, we have conducted radiativetransfer modelling of the ALMA data, showing that a Keplerian disc surrounding an O7 star, with a disc mass andradius of 12 Msun and 2000 AU reproduces the line and continuum data, further supporting our conclusion that
our observations have uncovered a Keplerian-like disc around an O-type star. This work is published in Johnston
et al. (2015).
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 15:00
Name: James Owen
Organisation: IAS, Princeton
Title: Vortices from low-mass planet formation in transition discs
Abstract:
Transition discs are protoplanetary discs that show evidence for dust trapping in their outer regions. Recent highangular resolution mm imaging of these discs has indicated that dust particles, as well being trapped radially,
are also concentrated in non-axisymmetric features, and it has been suggested that the dust particles aretrapped in a large scale vortex. Since the dust particles that naturally accumulate in transition disc dust traps
have Stokes numbers close to unity, there is naturally a large reservoir of ``pebbles'' in transition disc dust traps.
I will argue that the transition disc dust traps are prime sites for rapid ``pebble accretion'' onto low-massplanetary embryos. At the planetary accretion rates expected in nominal transition discs, the accretion
luminosity is sufficiently high to heat the surrounding disc to radii well outside the planet's Hill sphere. This
makes the disc locally baroclinic and can lead to vortex formation. I will present this ``new'' scenario for vortex
formation in transition discs and discuss the long term consequences, while arguing it is perhaps more naturalthan those scenarios discussed so far.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 15:20
Name: Michael Ireland
Organisation: Australian National University
Title: High Angular Resolution Mid-Infrared Imaging of Transitional Disks
Abstract:
Transitional and so-called pre-transitional disks consist of an optically thin inner disk and an optically thick outerdisk. In some disks, there is evidence for much more complex disk evolution than simply a cleared inner hole.
For example, in the case of Oph IRS 48, there is a dust trap in the outer disk and evidence for multiple cavity

47

sizes. We present high angular resolution observations of several disks with the Keck II telescope at infrared
wavelengths, primarily 3.7 microns, using adaptive optics and precision calibration techniques including
aperture mask interferometry. For Oph IRS 48 and HD 169142, we model the disks using RadMC-3D and showthat an azimuthally symmetric disk can model most but not all of the observed structure. In the case of HD
169142, a point-assymetry has been interpreted as direct luminosity from a planet. We discuss alternative
explanations from disk emission, showing why interpretation of high angular resolution observations ofluminous disk-bearing stars with single telescopes will always be difficult to interpret. A much more ambitious
instrument program such as the Planet Formation Imager will be needed to comprehensively disentnagle
complex disk evolution from planet formation.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 15:40
Name: Pablo Loren-Aguilar
Organisation: University of Exeter
Title: Toroidal vortices as a solution to the dust migration problem
Abstract:
We have identified a new type of dynamical dust–gas instability in protoplanetary discs that produces global
toroidal vortices, due to the process of dust settling. We have investigated the evolution of a dusty
protoplanetary disc with two different dust species (1 mm and 50 cm dust grains), under the presence of theinstability. We show how toroidal vortices, triggered by the interaction of mm grains with the gas, stop the radialmigration of metre-sized dust, potentially offering a natural and efficient solution to the dust migration problem.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 16:50
Name: Giovanni Rosotti
Organisation: Institute of Astronomy, University of Cambridge
Title: What is the minimum planet mass that creates observable signatures in proto-planetary discs?
Abstract:
I will discuss the prospects for observing how super-Earths and giant planetary cores shape the proto-planetary
disc. While previous theoretical work has shown how they affect the dust surface density much more than thegas one, no proper study has been conducted of what is the minimum planetary mass that produces observablesignatures. I address this problem by running multi-fluid gas and dust simulations and generating simulated
observations. I’ll highlight in particular how there exists a minimum planet mass that is able to produce apressure maximum outside its orbit and therefore a dust trap. Planet masses lower than the threshold can stillaffect the dust surface density, by creating traffic jams in the dust radial velocity; the minimum planet mass
detectable is roughly 10-15 Earth masses, but is a strong function of the disc temperature. Finally, I will discuss
how it is possible to have an estimate of the mass of the planet from the observations, which involves measuring
either the gap width in scattered light observations or the pressure maximum location in sub-mm images.

48

Time of talk: Friday 17:10
Name: Eiji Akiyama
Organisation: NAOJ
Title: Differential Grain Growth in the Spiral Structure of the LkHa 330 Disc
Abstract:
Grain growth represents an initial step toward planet formation since it involves the coagulation of
approximately micron-sized dust residing in protoplanetary discs around young stars. We have conducted Hband (1.6 um) linear polarimetric observations and 0.88 mm continuum interferometric observations toward atransitional disc around the intermediate-mass pre-main sequence star LkHa 330. The observations show a pairof asymmetric spiral arms in the disc. We discuss the origin of the spiral arms and suggest that a massive unseen
planet is the most plausible explanation based on recent global hydro simulations. The possibility of grain growthcausing the asymmetric structure of the spiral arms was investigated through the opacity index (beta) by plotting
the observed SED slope between 0.88 mm from our SMA observation and 1.3 mm from literature. The results
imply that grains are indistinguishable from ISM-like dust in the east side (beta ~ 2.0), but much smaller in thewest side (beta ~ 0.7), indicating differential grain growth or dust trapping in the spiral arms. Combining theresults of near-infrared and submillimetre observations, we find that the spiral arm is geometrically thick, andthat grains grow to millimeter size near the disc mid-plane. Future observations at centimeter wavelengths anddifferential polarization imaging in other bands (Y to K) with extreme AO imagers are required to understand
how large dust grains form and to further explore the dust distribution in the disc.
--------------------------------------------------------------------------------------------------------------------------------------------------Time of talk: Friday 17:30
Name: John Monnier
Organisation: University of Michigan
Title: GPI observations of Herbig Ae/Be stars
Abstract:
The discovery of transition disks around young stars has provided the opportunity to study planet formation insitu when giant planet formation and growth are most vigorous. Using the Gemini Planet Imager (GPI) in
differential polarimetry mode, we have begun a survey to characterize a statistically-significant sample of young
disks at each major stage of planet formation, from the youngest “full disk” stage and through pre-transition
and transition disk stages. GPI is ideal for this survey due to its unprecedented sensitivity to scattered lightemitted between 20-150 AU from the star, a region of the protoplanetary disk where giant planet formation is
known to occur. I will report initial observational results and radiative transfer modeling of a few well-known
systems. We explore how to combine ALMA and GPI imaging to measure radial variations in the disk’s grain size
distribution, outer disk gas pressure scale heights, and chemical snowlines.

49Poster submissions, by session

51

Poster
Ref.

SessionName

Organisation

Title

A1

Molecular
clouds

Jorge

Abreu
VicenteMax Planck Institute for
Astronomy

ALMA kinematic study of the Integral Shaped Filament in Orion

E1

Molecular
cloudsAhmad

Ali

University of Exeter

Modelling stellar feedback in clusters using Monte Carlo radiationhydrodynamics

E2

Molecular
clouds

Simon

Bihr

Max Planck Institute for
Astronomy

THOR - The HI, OH, Recombination Line survey of the Milky Way

A2

Molecular
cloudsDavid

Bresnahan

University of Central
Lancashire

The dense cores and filamentary structure of the molecular cloud inCorona Australis

A3

Molecular
cloudsVianeyCamacho

IRyA-UNAM

Understanding the energetics of clumps and dense cores.

A4

Molecular
cloudsGiuliana

Cosentino

University College London

Kinematics, SiO and CH3OH parsec-scale Emission in Filamentary
Infrared Dark Clouds.

A5

Molecular
clouds

Simon

Coudé

Université de Montréal

POL-2 & BISTRO: the SCUBA-2 polarimeter and the study of magnetismin star-forming regions

E3

Molecular
cloudsKevin

DouglasOkanagan College

The GALFA-HI Second Data Release

A6

Molecular
cloudsSergioAbrahamDzib Quijano

Max Planck Institute for
Astronomy

A comprehensive Galactic plane radio wavelength star formation
surveyA7

Molecular
cloudsErica

Fogerty

University of Rochester

Molecular cloud formation in high shear, magnetized colliding flows

52

Poster
Ref.

SessionName

Organisation

Title

A8

Molecular
cloudsKathrynGoldsmith

University of Leeds

The interaction of astrophysical flows with clouds and filaments

A9

Molecular
clouds

Munan

Gong

Princeton University

Simulating CO formation in realistic star formation environments

A10

Molecular
cloudsSebastian

Haid

University of Cologne

The consequences of stellar feedback on molecular clouds

A11

Molecular
cloudsKazunari

Iwasaki

Doshisha University

Formation of massive filamentary molecular clouds by shockcompression

A12

Molecular
clouds

Venu

KalariUniversidad de Chile

Feedback and triggering on the molecular clouds in R136

A13

Molecular
cloudsIvaylaKalcheva

University of Leeds

Properties of the CORNISH-North UCHII sample

A14

Molecular
clouds

Jared

Keown

University of Victoria

Characterizing Starless Cores, Protostars, and Filaments in Cepheus

A15

Molecular
cloudsJeong-Gyu

Kim

Seoul National University

Disruption of Molecular Clouds by Radiative Feedback from Massive
Stars

A16

Molecular
cloudsAlexander

Lodge

UCLan

Properties of pre-stellar cores observed using the Herschel SPIRE
Instrument

A17

Molecular
cloudsJingqi

Miao

Kent University

The roles of chemical feedback in the evolution of molecular clouds in
PDRs and HII regions

A18

Molecular
cloudsOmnarayani

Nayak

Johns Hopkins University

Relating Young Stars Imaged by Spitzer and Hubble to the CO
Molecular Gas Observed with ALMA in 30 Doradus and N159 West

A19

Molecular
cloudsJan

OrkiszObservatoire de Paris / IRAM

Turbulence versus star formation efficiency in Orion

53

Poster
Ref.

SessionName

Organisation

Title

A20

Molecular
cloudsHsi-AnPan

Academia Sinica Institute of
Astronomy and Astrophysics(ASIAA)The Role of GMC Observations in the Big Picture: Effects of Galactic
Disc Inclination and Resolution on Observed GMC Properties andLarson’s Scaling Relations

A21

Molecular
cloudsLiubinPan

Harvard-Smithsonian Center
for Astrophysics

Compressibility and density fluctuations in supernova-driven
turbulence in molecular clouds

A22

Molecular
cloudsJulianPittard

University of Leeds

MHD simulation of stellar feedback in a filamentary molecular cloudformed by the thermal instability

A23

Molecular
cloudsDanielSeifried

University of Cologne

Zooming into the dynamical and chemical evolution of molecular
clouds

E4

Molecular
cloudsNeha

SharmaARIES-Nainital-India

Optical polarimetric and molecular line observations of two brightrimmed clouds, BRC 18 and BRC 38.

A24

Molecular
clouds

LaszloSzucs

Max Planck Institute forExtraterrestrial Physics

On the caveats of tracing molecular gas with CO emission

A25

Molecular
cloudsGwenllian

Williams

Cardiff University

What can filament dynamics tell us about core formation?

E5

Molecular
cloudsChang

Won Lee

Korea Astronomy and Space
Science Institute

TRAO multi-beam Survey of Nearby Molecular Clouds

A26

Molecular
cloudsSac Nicte

XiomaraSerranoMedinaMax Planck Intitute forRadioastronomy

Turbulence in the Orion Nebula

B1

Protostellar
cores

JosephBookerUniversity of Toledo

HST Scattered Light Imaging of Orion Protostars: Do Outflows Halt
Infall?

B2

Protostellar
cores

James

Di Francesco

National Research Council of
CanadaThe Next Generation Very Large Array

54

Poster
Ref.

SessionName

Organisation

Title

B3

Protostellar
cores

Mathilde

Gaudel

CEA Saclay

Rotation in protostellar envelopes of CALYPSO sources

B4

Protostellar
cores

Il-GyoJeong

Korea Astronomy and Space
Science InstituteStar forming activities in the vicinity of the HII region G84.9+0.5

B5

Protostellar
cores

Hyunwoo

Kang

Korea Astronomy and Space
Science Institute

Investigation of simultaneous observation results of water and class I
methanol masers toward class II methanol maser sources

B6

Protostellar
cores

Hyun-Jeong

Kim

Seoul National University

Massive Young Stellar Objects with H2 Outflows in Infrared Dark CloudCore MSXDC G53.11+00.05 MM1

B7Protostellar
cores

Kee-Tae

Kim

Korea Astronomy and Space
Science Institute

KVN Studies of Water and Methanol Masers in Massive YSOs

B8

Protostellar
cores

RajikaKuruwita

Australian National
University

Jets from forming binary star systems

E6

Protostellar
cores

Bilal

Ladjelate

CEA-Laboratoire AIM-ParisSaclay

Star-formation in the Ophiuchus Molecular Cloud: Similarities anddiversity

B9

Protostellar
cores

PierreMarchand

CRAL-ENS Lyon

Non ideal MHD and chemistry in star formation

B10

Protostellar
cores

Chris

Mowat

University of Exeter

The JCMT Gould Belt Survey: A First Look at SCUBA-2 Observations of
the Lupus I Molecular Cloud

B11

Protostellar
cores

ZsofiaNagy

University of Toledo - USA

Measuring rotation in protostellar envelopes: ALMA Observations ofEdge-On Orion Protostars

B12

Protostellar
cores

Raul

Naranjo
RomeroInstituto deRadioastronomia y
Astrofisica

Hierarchical gravitational fragmentation. I. Collapsing cores withincollapsing clouds

55Poster
Ref.

SessionName

Organisation

Title

B13

Protostellar
cores

Fernando

OlguinChoupay

University of Leeds

The physical properties of the prototypical MYSO GL 2591

B14

Protostellar
cores

HowardSmith

Harvard-Smithsonian Centre
for Astrophysics

Unraveling YSO Clusters in Protostellar Cores and IRDCs

B15

Protostellar
cores

RachaelSpowage

Cardiff University

Investigating the presence of a transition to coherence in (magneto)hydrodynamical simulations

B16

Protostellar
cores

Jacob

Ward

Keele University

Integral field spectroscopy of massive YSOs in the Small Magellanic
Cloud

B17

Protostellar
cores

Jennifer

WisemanNASA Goddard Space Flight
CenterA Newly Discovered Ammonia Source With Peculiar Chemistry Near the
HH 111/HH 121 Protostellar System

B18

Protostellar
cores

James

Wurster

University of Exeter

How non-ideal MHD affects the evolution of the environment around aforming protostar

B19

Protostellar
cores

Yao-LunYang

The University of Texas atAustinThe Class 0 Protostar BHR71: Herschel Observations and Dust
Continuum Models

B20

Protostellar
cores

AlisonYoung

University of Exeter

Hydrodynamic and radiative transfer modelling of first hydrostatic core
candidates

B21

Protostellar
cores

Ka Ho

Yuen

The Chinese University ofHong Kong

Divergence between dynamic and spatial field-density variance during
proto-star core formation in interstellar media

C1

Protostars &clusters

MortenAndersenGemini ObservatoriesGemini SouthThe very low-mass stellar content of the young supermassive Galactic
star cluster Westerlund 1

C2

Protostars &clusters

Costanza

Argiroffi

DiFC - University of Palermo

X-ray Doppler shift from TW Hya: constraints on the accretion process

56

Poster
Ref.

SessionName

Organisation

Title

C3

Protostars &clusters

Becky

ArnoldUniversity of Sheffield

Binary clusters of stars

C4

Protostars &clusters

CameronBell

ETH Zurich

A stellar census of the 32 Ori moving group

C5

Protostars &clusters

Tyler

BourkeSKA Observatory

Revealing the jets in the BHR71 protostellar system

C6

Protostars &clusters

Ross

Burns

JIVE

Water masers in a jet-driven bowshock: Episodic ejection from a
massive young stellar object

C7

Protostars &clusters

JustynCampbellWhite

University of Kent

Classifying HII Regions Using Shape Analysis of IR Bubbles

C8

Protostars &clusters

Zhiwei

Chen

Ruhr-University Bochum

Stellar feedback of massive star formation in M17

C9

Protostars &clusters

ClaireEsau

The University of SheffieldNo evidence for primordial mass segregation

C10

Protostars &clusters

Shane

Fogerty

University of Rochester

Silicate dust grain composition in the interstellar medium

C11

Protostars &clusters

Dirk

Froebrich

University of Kent

Photometric Monitoring of nearby young Clusters as a Citizen Science
Project

C12

Protostars &clusters

Abigail

Frost

University of Leeds

A MIDI/VISIR Study of an MYSO

C13

Protostars &clusters

Phillip

Galli

Institute of Astronomy,
Geophysics and Atmospheric
Sciences, Brazil

A VLBI Distance Determination to the Taurus-Star Forming Region

57

Poster
Ref.

SessionName

Organisation

Title

C14

Protostars &clusters

Simon

Goodwin

University of Sheffield

Prestellar sources in Serpens

C15

Protostars &clusters

Dan

Griffiths

University of Sheffield

Massive Wide Binaries as Tracers for the Dynamical History of Stellar
Regions

C16

Protostars &clusters

Mario
Giuseppe

Guarcello

INAF - Osservatorio
Astronomico di Palermo

Photoevaporation and close encounters: how the environment around
Cygnus~ OB2 affects the evolution of protoplanetary disks

C17

Protostars &clusters

Mario
Giuseppe

Guarcello

INAF - Osservatorio
Astronomico di Palermo

Time resolved X-ray spectral analysis of class II YSOs in NGC2264
during optical dips and bursts

C18

Protostars &clusters

Zhen

Guo

KIAA-PKU

Evidence of star-disk interaction on a classical T Tauri star

C19

Protostars &clustersDavid

Guszejnov

CaltechThe Minimum Physics of Star Formation

C20

Protostars &clusters

Sasha

Hinkley

University of Exeter

New Extreme-Mass Ratio Systems at 10 Million Years

C21

Protostars &clusters

MichaelJones

University of Exeter

Predicting the dependence of stellar properties on environment.

C22

Protostars &clusters

Venu

KalariUniversidad de Chile

Star formation processes may be affected by metallicity

C23

Protostars &clusters

Christine

Koepferl

University of St Andrews

Insights from Synthetic Star-forming Regions Measuring Star-formation
Rates and Gas/Dust Properties

C24

Protostars &clusters

Nanda

Kumar

Centre for Astrophysics University of Hertfordshire

Highly variable young massive stars in ATLASGAL clumps

C25

Protostars &clusters

Masanobu

Kunitomo

Nagoya University

On the effect of planet formation on stellar surface composition

58

Poster
Ref.

SessionName

Organisation

Title

C26

Protostars &clusters

Alejandro

Lopez

Instituto deRadioastronomia y
Astrofisica- UNAM

Angular momentum in bipolar outflows

C27

Protostars &clusters

Steve

Mairs

University of Victoria

How Do Protostars Assemble Mass? A Sub-Millimetre (JCMT) Variability
Survey of Deeply Embedded Protostars

C28

Protostars &clusters

Sally

Makin

University of Kent

Star formation in Cygnus-X: hunting young stellar outflows in theinfrared with UWISH2

C29

Protostars &clusters

Brian

Mazur

University of Toledo

A Spectroscopic Survey of 100-1000 AU Companions to Orion YSOs

C30

Protostars &clusters

StefanMeingast

University of Vienna

VISION - Vienna survey in Orion

C31

Protostars &clusters

Georgios

Pantolmos

University of Exeter

Magnetic braking of cool stars: dependence on coronal temperature

C32

Protostars &clusters

Mark

PecautRockhurst University

Star Formation History of the Scorpius-Centaurus OB Association

C33

Protostars &clusters

MonikaPetrGotzens

European Southern
Observatory

The VISTA Orion mini-survey: Young Stellar Objects in Orion B

C34

Protostars &clusters

RobertPomohaci

University of Leeds

Near-IR spectroscopy of Massive Young Stelar Objects

C35

Protostars &clusters

Simon

PurserUniversity of Leeds

A search for ionised jets towards massive protostars

C36

Protostars &clusters

Tae-Soo

Pyo

Subaru Telescope / NAOJ

Ejection of Knots and Photometric Variability in DG Tau 30 years

59

E7

Protostars &clusters

Carolina
Berenice

Rodríguez
Garza

IRyA-UNAMFirst observations of Galactic massive star-forming regions taken with
the Mexican Large Millimeter Telescope

C37

Protostars &clusters

ChristianSchneider

ESA/ESTEC

Hot jets from young, cool stars

C38

Protostars &clusters

Priya

Shah

Maluana Azad National Urdu
University- Hyderabad

Triggered Star Formation at different spatial scales in NGC 281

C39

Protostars &clusters

Romas

Smilgys

University of St Andrews

Formation of stellar clusters in Galactic flows

C40

Protostars &clusters

Sonu

TabithaPaulsonIndian Institute of Space
Science and TechnologyTrivandrum

Probing High Mass stars with 6.7 GHz Methanol Masers

C41

Protostars &clusters

Mauricio

Tapia

Instituto de Astronomia UNAM - Ensenada - Mexico

NGC 6334 V revisited: The nature of the young elongated infrared
nebulaE8

Protostars &clusters

Benny

Tsang

The University of Texas atAustinRadiation Pressure Feedback in Super Star Cluster Formation

C42

Protostars &clusters

ElaineWinstonSmithsonian AstrophysicalObservatory

TARDISS: Time and Relative Dimensions in Serpens South

C43

Protostars &clusters

Scott

Wolk

Harvard-Smithsonian Center
for Astrophysics

Discovery of Two New Nearby Associations of Young Stars

C44

Protostars &clusters

Eleonora

Zari

Leiden Observatory

Maximum likelihood membership analysis of OB associations with Gaia

D1

Discs

AmeliaBayo

Universidad de Valparaiso

In depth view of the debris disk around TWA7

D2

Discs

Dominika

Boneberg

Institute of AstronomyCambridge

The midplane conditions of protoplanetary discs

D3

Discs

ClaireDavies

University of Exeter

Revealing the structure of the inner disk rim with CHARA

60

Poster
Ref.

SessionName

Organisation

Title

D4

Discs

Tom

DouglasUniversity of Exeter

Radiation-hydrodynamic simulations of line driven disc-winds around
MYSOs

D5

Discs

DuncanForganUniversity of St Andrews

Detecting Filaments and Spiral Structures in Smoothed Particle
Hydrodynamic Simulations of Star Formation

D6

Discs

Gesa

H.-M.
Bertrang

Universidad de Chile &Universidad Diego Portales

How to interpret observations of magnetic fields in protoplanetary
disks

D7

Discs

EdwardHone

University of Exeter

Unveiling the sub-AU kinematics of the Herbig B[e] star MWC297

D8

Discs

John

Ilee

Institute of Astronomy Cambridge

G11.92—0.61 MM1: A disc around a young massive star?

D9

Discs

Dylan

Kee

University of Tübingen

Line-Driven Ablation of Star Forming Disks

D10

Discs

Jacques

KluskaUniversity of Exeter

What does the disks inner rim look like? Images and implications fromthe interferometric VLTI/PIONIER survey of Herbig Ae/Be Objects.

D11

Discs

Alexander

Kreplin

University of Exeter

Resolving the inner disk of UX Orionis

D12

Discs

FelipeNavarete

University of São Paulo

Jets and disks driven by High-Mass YSOs revealed through 3DSpectroscopy

D13

Discs

Rhana

Nicholson

LJMU- Astrophysics ResearchInstitute

Supernova enrichment of planetary systems in unusual star clusters

D14

Discs

Johan

Olofsson

IFA - Universidad de
Valparaiso

Azimuthal asymmetries in the debris disk around HD61005

D15

Discs

Jon

Rees

University of Exeter

Environmental impact on disc lifetimes

D16

Discs

Julia

Roquette

Universidade Federal de
Minas Gerais (UFMG)

Near-Infrared variability of disk-bearing stars in Cygnus OB2

61

D17

Discs

AlbertoSanna

Max-Planck-Institut fuer
Radioastronomie

Gas dynamics driven by a massive YSO: Observations confront Theory

D18

Discs

AndreySobolev

Ural Federal University Astronomical Observatory

Towards detecting methanol emission in low-mass protoplanetary discs
with ALMA: The role of non-LTE excitation

D19

Discs

Yuhei

TakagiNational Astronomical
Observatory of Japan

Evolution timescale of circumstellar disks in nearby star forming
regions

D20

Discs

Sierk

van
Terwisga

Leiden University

A Short Cut to Rings – resolved ALMA images of CN rings in Lupus

D21

Discs

Merel

van't Hoff

Leiden Observatory

Robustness of N2H+ as tracer of the CO snowline

D22

Discs

Matthew

Willson

University of Exeter

Sparse Aperture Masking Interferometry Survey of Transitional Disks

62

Delegate List
AliciaAarnioUniversity of Michigan

aarnio@umich.edu

Jorge

Abreu Vicente

Max Planck Institute for Astronomy

abreu@mpia.de

Eiji

AkiyamaNAOJ

eiji.akiyama@nao.ac.jp

RichardAlexander

University of Leicesterrichard.alexander@leicester.ac.uk

Ahmad

Ali

University of Exeter

aali@astro.ex.ac.uk

Joao

Alves

University of Vienna

joao.alves@univie.ac.at

MortenAndersenmanderse@gemini.edu

Philippe

AndréGemini Observatories- GeminiSouth
CEA Saclay

Costanza

Argiroffi

DiFC - University of Palermo

argi@astropa.unipa.it

Becky

ArnoldUniversity of Sheffieldr.j.arnold.uk@gmail.com

YusukeAso

The University of Tokyo

yusuke@naoj.org

Isabelle

Baraffe

University of Exeter

I.Baraffe@exeter.ac.uk

Matthew

Bate

University of Exeter

mbate@astro.ex.ac.uk

AmeliaBayo

Universidad de Valparaiso

amelia.bayo@uv.cl

CameronBell

ETH Zurichcbell@phys.ethz.ch

Simon

Bihr

Max Planck Institute for Astronomy

bihr@mpia.de

Dominika

Boneberg

Institute of Astronomy- Cambridge

dmrb3@ast.cam.ac.uk

JosephBookerUniversity of Toledo

joe@neoturbine.net

Tyler

BourkeSKA Observatory

t.bourke@skatelescope.org

AndreaBracco

CEA, Saclay

andrea.bracco@cea.fr

David

Bresnahan

University of Central Lancashire

dwbresnahan@uclan.ac.uk

Chris

Brunt

University of Exeter

brunt@astro.ex.ac.uk

Ross

Burns

JIVE

RossBurns88@googlemail.com

HaroldButnerJames Madison University

butnerhm@jmu.edu

Nuria

Calvet

University of Michigan

ncalvet@umich.edu

VianeyCamacho

IRyA-UNAM

v.camacho@crya.unam.mx

JustynCampbellWhite
Chabrier

University of Kent

jc849@kent.ac.uk

University of Exeter

chabrier@ens-lyon.fr

Huei-Ru
VivienZhiweiChen

National Tsing Hua University

hchen@phys.nthu.edu.tw

Chen

Ruhr-University Bochum

zchen@astro.rub.de

SeamusClarkeCardiff University

seamus.clarke@astro.cf.ac.uk

BenoîtCommerçon

CNRS

benoit.commercon@ens-lyon.fr

Giuliana

Cosentino

University College London

giuliana.cosentino.15@ucl.ac.uk

Simon

Coudé

Université de Montréal

coude@astro.umontreal.ca

ClaireDavies

University of Exeter

cdavies@astro.ex.ac.uk

Guido

De Marchi

European Space Agency

gdemarchi@esa.int

James

Di Francesco

james.difrancesco@nrc-cnrc.gc.ca

Sami

Dib

National Research Council of
CanadaNiels Bohr Institute

Kevin

DouglasOkanagan College

kdouglas@okanagan.bc.ca

TomDouglasUniversity of Exeter

t.douglas@exeter.ac.uk

Emily

DrabekMaunder

Imperial College London

e.drabek-maunder@imperial.ac.uk

Gillespandre@cea.fr

sami.dib@gmail.com

Janet

Drew

University of Hertfordshire

j.drew@herts.ac.uk

Ana

Duarte Cabral

University of Exeter

adc@astro.ex.ac.uk

SergioAbrahamClaireDzib Quijano

Max Planck Institute for Astronomy

sdzib@mpifr-bonn.mpg.de

Esau

The University of Sheffieldc.esau@shef.ac.uk

Catherine

Espaillat

Boston University

cce@bu.edu

Marc

Evans

University of Leeds

py09mge@leeds.ac.uk

StewartEyres

University of Central Lancashire

spseyres@uclan.ac.uk

Carlo

Felice Manara

ESA/ESTEC

cmanara@cosmos.esa.int

Adam

FinleyUniversity of Exeter

adam.finley.94@googlemail.com

Erica

Fogerty

University of Rochester

erica@pas.rochester.edu

Shane

Fogerty

University of Rochester

sfogerty@pas.rochester.edu

JanForbrich

University of Vienna

jan.forbrich@univie.ac.atDuncanForganUniversity of St Andrews

dhf3@st-andrews.ac.uk

Dirk

Froebrich

University of Kent

df@star.kent.ac.uk

Abigail

Frost

University of Leeds

pyajf@leeds.ac.uk

Phillip

Galliphillip.galli@iag.usp.br

Mathilde

GaudelInstitute of Astronomy, Geophysics
and Atmospheric Sciences, Brazil
CEA Saclay

Sam

Geen

CEA Saclay

samuel.geen@cea.fr

Simon

Gloverglover@uni-heidelberg.de

KathrynGoldsmithInstitute for Theoretical
Astrophysics - University of
Heidelberg
University of Leeds

Munan

Gong

Princeton University

munan@princeton.edu

Simon

Goodwin

University of Sheffields.goodwin@sheffield.ac.uk

Dan

Griffiths

University of Sheffieldd.griffiths@sheffield.ac.uk

JosefaGrossschedl

josefa.elisabeth.grossschedl@univie.ac.at

Mario
Giuseppe
Zhen

Guarcello
Guo

University of Vienna-Institute for
Astrophysics
INAF - Osservatorio Astronomico diPalermo
KIAA-PKUDavid

Guszejnov

Caltechguszejnov@caltech.edu

Gesa

Universidad de Chile & Universidad
Diego Portales
University of Cologne

bertrang@das.uchile.cl

SebastianH.-M.
Bertrang
Haid

Tim

Harries

University of Exeter

th@astro.ex.ac.uk

LeeHartmann

University of Michigan

lhartm@umich.edu

Jennifer

HatchellUniversity of Exeter

jh278@exeter.ac.uk

JonathanHenshaw

Liverpool John Moores University

j.d.henshaw@ljmu.ac.uk

Sasha

Hinkley

University of Exeter

shinkley@gmail.com

EdwardHone

University of Exeter

ehone@astro.ex.ac.uk

John

Ilee

Institute of Astronomy - Cambridge

jdilee@ast.cam.ac.uk

MichaelIreland

Australian National University

michael.ireland@anu.edu.au

Kazunari

Iwasaki

Doshisha University

kiwasaki@mail.doshisha.ac.jp

Il-GyoJeongigjeong@kasi.re.kr

Katharine

Johnston

Korea Astronomy and Space
Science Institute
University of Leeds

MichaelJones

University of Exeter

mjones@astro.ex.ac.uk

64

mathilde.gaudel@cea.fr

pykjag@leeds.ac.uk

mguarce@astropa.unipa.it
guozhen9057@hotmail.com

haid@ph1.uni-koeln.dek.g.johnston@leeds.ac.uk

JouniKainulainen

Max Planck Institute for Astronomy

jtkainul@mpia.de

Venu

KalariUniversidad de Chile

venukalari@gmail.com

IvaylaKalcheva

University of Leeds

pyiek@leeds.ac.uk

HyunwooKangorionkhw@kasi.re.kr

Dylan

Kee

Korea Astronomy and Space
Science Institute
University of Tübingen

Jared

Keown

University of Victoria

jkeown@uvic.ca

Eric

Keto

eketo@cfa.harvard.edu

Hyun-Jeong

Kim

Harvard-Smithsonian Center for
Astrophysics
Seoul National University

Jeong-Gyu

Kim

Seoul National University

jgkim@astro.snu.ac.kr

Kee-TaeKim

ktkim@kasi.re.kr

Jacques

KluskaKorea Astronomy and Space
Science Institute
University of Exeter

MasatoKobayashi

Nagoya University

masato.kobayashi@nagoya-u.jp

Christine

Koepferl

University of St Andrews

cmk8@st-andrews.ac.uk

Vera

Könyvesvera.konyves@gmail.com

StefanKraus

Lab. AIM- Paris-Saclay- CEA/SaclayFrance
University of Exeter

Alexander

Kreplin

University of Exeter

akreplin@astro.ex.ac.uk

Nanda

Kumar

n.kumar@herts.ac.uk

Masanobu

Kunitomo

Centre for Astrophysics - University
of Hertfordshire
Nagoya University

RajikaKuruwita

Australian National University

kunitomo.masanobu@c.mbox.nagoyau.ac.jp
rajika.kuruwita@anu.edu.au

Bilal

Ladjelate

CEA-Laboratoire AIM-Paris-Saclay

bilal.ladjelate@cea.fr

Benjamin

Lewis

University of Exeter

blewis@astro.ex.ac.uk

Alexander

Lodge

UCLan

alodge@uclan.ac.uk

Oliver

Lomax

Cardiff University

oliver.lomax@astro.cf.ac.uk

Alejandro

Lopez

j.lopez@crya.unam.mx

Pablo

Loren-Aguilar

Instituto de Radioastronomia y
Astrofisica- UNAM
University of Exeter

PhilipLucas

University of Hertfordshire

p.w.lucas@herts.ac.uk

Steve

Mairs

University of Victoria

smairs@uvic.ca

Sally

Makin

University of Kent

svm67@kent.ac.uk

PierreMarchand

CRAL-ENS Lyon

pierre.marchand@ens-lyon.fr

Sean

Matt

University of Exeter

s.matt@exeter.ac.uk

AnaëlleMaury

CEA-Laboratoire AIM-Paris-Saclay

anaelle.maury@cea.fr

Brian

Mazur

University of Toledo

brian.mazur@rockets.utoledo.edu

Mark

McCaughrean

European Space Agency

mark@mccaughrean.net

Melissa

McClureEuropean Southern Observatory

mmcclure@eso.org

ThomasMegeath

University of Toledo

tommegeath@gmail.com

StefanMeingast

University of Vienna

stefan.meingast@univie.ac.at

Jingqi

Miao

Kent University

j.miao@kent.ac.uk

JohnMonnier

University of Michigan

monnier@umich.edu

SamMorrell

University of Exeter

smorrell@astro.ex.ac.uk

JosephMottram

Max Planck Institute for Astronomy

mottram@mpia.de

Chris

Mowat

University of Exeter

cm365@exeter.ac.uk

Nadia

Murillo

Leiden Observatory

nmurillo@strw.leidenuniv.nl

65

nathaniel-dylan.kee@uni-tuebingen.de

hjkim@astro.snu.ac.kr

jkluska@astro.ex.ac.uk

skraus@astro.ex.ac.uk

pablo@astro.ex.ac.uk

Zsofia

Nagy

University of Toledo - USAzsofia.nagy.astro@gmail.com

Raul

Instituto de Radioastronomia y
Astrofisica
University of São Paulor.naranjo@irya.unam.mx

FelipeNaranjo
RomeroNavarete

Omnarayani

Nayak

Johns Hopkins University

onayak1@jhu.edu

TimNaylorUniversity of Exeter

t.naylor@exeter.ac.uk

Rhana

Nicholson

R.B.Nicholson@2011.ljmu.ac.uk

StellaOffner

LJMU- Astrophysics ResearchInstitute
UMass Amherst

Fernando

University of Leeds

pyfao@leeds.ac.uk

JoanaOlguinChoupay
Oliveira

Keele University

j.oliveira@keele.ac.uk

Johan

Olofsson

IFA - Universidad de Valparaiso

johan.olofsson@uv.clJanOrkiszObservatoire de Paris / IRAM

jan.orkisz@ens.fr

VolkerUniversity of Cologne

ossk@ph1.uni-koeln.deJames

OssenkopfOkada
Owen

IAS, Princeton

jamesowen@cantab.net

Hsi-AnPanhapan@asiaa.sinica.edu.tw

LiubinPan

Georgios

Pantolmos

Academia Sinica Institute of
Astronomy and Astrophysics(ASIAA)
Harvard-Smithsonian Center for
Astrophysics
University of Exeter

RichardParkerLiverpool John Moores University

R.J.Parker@ljmu.ac.uk

Kate

PattleUniversity of Central Lancashire

kpattle@uclan.ac.uk

MarkPecautRockhurst University

Mark.Pecaut@Rockhurst.edu

Nicolas

PerettoCardiff University

Nicolas.Peretto@astro.cf.ac.uk

MonikaPetr-Gotzens

European Southern Observatory

mpetr@eso.org

JulianPittard

University of Leeds

jmp@ast.leeds.ac.uk

RobertPomohaci

University of Leeds

pyrp@leeds.ac.uk

Simon

PurserUniversity of Leeds

pysjp@leeds.ac.uk

Tae-Soo

Pyo

Subaru Telescope / NAOJ

pyo@naoj.org

Jon

Rees

University of Exeter

jmr215@exeter.ac.uk

Megan

Reitermreiter@umich.edu

AlvaroRibas

Department of AstronomyUniversity of Michigan
Boston University

Isabelle

Ristorcelli

IRAP/CNRS-UPS

Isabelle.Ristorcelli@irap.omp.eu

Alana

ESA

alana.rivera@sciops.esa.int

Carolina
Berenice
Julia

RiveraIngraham
Rodríguez
Garza
Roquette

IRyA-UNAM

carol.gza@gmail.com
juliaroquette@gmail.com

Giovanni

Rosotti

Cynthia

Saad

Universidade Federal de Minas
Gerais (UFMG)
Institute of Astronomy, Universityof Cambridge
American University of Beirut

Sarah

Sadavoy

Max Planck Institute for Astronomy

sadavoy@mpia-hd.mpg.deStuartSale

University of Exeter

ssale@astro.ex.ac.uk

AlbertoSanna

asanna@mpifr-bonn.mpg.de

ChristianSchneider

Max-Planck-Institut fuer
Radioastronomie
ESA/ESTEC

66

navarete@usp.br

soffner@astro.umass.edu

lpan@cfa.harvard.edu
gp323@exeter.ac.uk

aribas@bu.edu

rosotti@ast.cam.ac.uk
crs07@mail.aub.edu

cschneid@cosmos.esa.int

DanielSeifried

University of Cologne

seifried@ph1.uni-koeln.de

Priya

Shah

priya.hasan@gmail.comm

Neha

SharmaMaluana Azad National Urdu
University- Hyderabad
ARIES-Nainital-India

Romas

Smilgys

University of St Andrews

rs202@st-andrews.ac.uk

HowardSmithhsmith@cfa.harvard.edu

MichaelSmith

Harvard-Smithsonian Centre for
Astrophysics
University of Kent

AndreySobolev

Andrej.Sobolev@urfu.ru

RachaelSpowage

Ural Federal University Astronomical Observatory
Cardiff University

LaszloSzucs

laszlo.szucs@mpe.mpg.de

Sonu
Yuhei

TabithaPaulsonTakagi

Mauricio

Tapia

Kengo

TomidaMax Planck Institute forExtraterrestrial Physics
Indian Institute of Space Scienceand Technology-Trivandrum
National Astronomical Observatoryof Japan
Instituto de Astronomia - UNAM Ensenada - Mexico
Osaka University

Benny

Tsang

The University of Texas at Austin

bthtsang@astro.as.utexas.edu

YusukeTsukamoto

RIKEN

yusuke.tsukamoto@riken.jp

James

Urquhart

University of Kent

j.s.urquhart@gmail.com

Sierk

van Terwisga

Leiden University

terwisga@strw.leidenuniv.nl

Merel

van't Hoff

Leiden Observatory

vthoff@strw.leidenuniv.nl

Neil

VaytetNiels Bohr Instituteneil.vaytet@nbi.ku.dk

EnriqueUNAM

e.vazquez@crya.unam.mx

Laura

VazquezSemadeni
Venutilvenuti@astropa.unipa.it

Stefanie

Walch

INAF - Osservatorio Astronomico diPalermoUniversity of Cologne

Jacob

Ward

Keele University

j.l.ward@keele.ac.uk

Gwenllian

Williams

Cardiff University

williamsgm8@cf.ac.uk

Matthew

Willson

University of Exeter

maw214@exeter.ac.uk

Tom

WilsonUniversity of Exeter

tjw207@exeter.ac.uk

ElaineWinstonelaine.winston@cfa.harvard.edu

Jennifer

WisemanSmithsonian AstrophysicalObservatory
NASA Goddard Space Flight Center

Scott

Wolk

swolk@cfa.harvard.edu

Chang

Won Lee

Kenny

Wood

Harvard-Smithsonian Center for
Astrophysics
Korea Astronomy and Space
Science Institute
University of St Andrews

Paul

Woods

Nature Astronomy

paul.woods@nature.com

Christopher

WrightUNSW Canberra

c.wright@adfa.edu.au

Nick

WrightKeele University

n.j.wright@keele.ac.uk

James

Wurster

University of Exeter

j.wurster@exeter.ac.uk

Sac Nicte

XiomaraSerranoMedinaYang

Max Planck Intitute forRadioastronomy

smedina@mpifr-bonn.mpg.de

The University of Texas at Austin

yaolun@astro.as.utexas.edu

Yao-Lun67

pathakneha.sharma@gmail.com

m.d.smith@kent.ac.uk

SpowageRL@cardiff.ac.uk

sonutabitha@gmail.com
yuhei.takagi@nao.ac.jp
mt@astrosen.unam.mx
tomida@vega.ess.sci.osaka-u.ac.jp

walch@ph1.uni-koeln.dejennifer.wiseman@nasa.gov

cwl@kasi.re.kr
kw25@st-andrews.ac.uk

AlisonYoung

University of Exeter

ay227@exeter.ac.uk

Ka Ho

Yuen

khyuen@phy.cuhk.edu.hk

Eleonora

Zari

The Chinese University of Hong
Kong
Leiden Observatory

YapengZhang

The Chinese University of Hong
Kong

ypzhang@phy.cuhk.edu.hk

68

zariem@strw.leidenuniv.nl