SFN$303$No.19+28$ 2018/05/11

SFN$303$No.19+28$ 2018/05/11 19. Inside+Out$Planet$Formation.$IV.$Pebble$Evolution$and$Planet$Formation$Timescales 20. The$Herschel+PACS$legacy$of$low+mass$protostars:$Properties$of$warm$and$hot$gas$and$its$ origin$in$far+uv$illuminated$shocks 21. Core$Emergence$in$a$Massive$Infrared$Dark$Cloud:$A$Comparison$Between$Mid+IR$ Extinction$and$1.3$mm$Emission 22. Characterization$of$methanol$as$a$magnetic$field$tracer$in$star+forming$regions 23. Near+infrared$study$of$new$embedded$clusters$in$the$Carina$complex 24. The$physical$and$chemical$structure$of$Sagittarius$B2.$III.$Radiative$transfer$simulations$of$ the$hot$core$sgrb2(m)$for$methyl$cyanide 25. Seeds$of$Life$in$Space$(SOLIS).$III.$Zooming$into$the$methanol$peak$of$the$pre+stellar$core$ L1544 26. Spiral$density$waves$and$vertical$circulation$in$protoplanetary$discs 27. Study$of$the$filamentary$infrared$dark$cloud$G192.76+00.10$in$the$S254+S258$OB$ complex 28. Orbital$Motion$of$Young$Binaries$in$Ophiuchus$and$Upper$Centaurus+Lupus

#21 Core%Emergence%in%a%Massive%Infrared%Dark%Cloud:%A%Comparison% Between%Mid=IR%Extinction%and%1.3%mm%Emission% ALMA mm ALMA 10 5 Mo IRDC G28.37%+%0.07 12m array 86 IRDC

MIREX ALMA Σ>0.2-g-cm12 Spitzer-IRAC-8μm dark-region MIREX Σ ALMA Σ ALMA pre1stellar-core- massivepre1stellar-core ALMA FIg. 1 :MIREX ALMA 1.3-mm Contours:-ALMA-1.3-mm-continuum-mosaic. The-two-red-contours-highlight-SNR-=-3-and-10.

Fig.%2 Σ ALMA1.3%mm / / IRDC Σ Fig.%4

1.3mm protostellar-cmf pre1 stellar-cmf fdg 50 fdg ε* 5 8 1.3mm protostellar-cores IRDC εff McKee Tan 2003 1 (ε core ) 50 ε ff fdg 10

#25 Seeds%of%Life%in%Space%(SOLIS).%III.%Zooming%into%the%methanol% peak%of%the%pre;stellar%core%l1544 Introduction (CH 3 OH) cold%dense%clouds CO L1544 pre;stellar%core(n~2x10^6%cm^;3) Observation NOEMA beam%:5.71 x3.86 20 IRAM%30m NOEMA (CH 3 OH) Fig.%1 IRAM%30m color%scale%:ch3oh 250%µm%dust%continuum

Results Fig.22 The2white2contours2:21.22mm2dust2continuum2emission The2yellow2cross2shows2the2dust2emission2peak. Fig.23 NOEMA+30m NOEMA (FIg.2) NOEMA+30m (Fig.23)

Results Fig."4 Velocity"dispersions"of"theA+methanol"line. Fig."7 Fig."13 7"km"s&1"pc&1 (Fig."7) (Fig."4) pre&stellar"core Herschel FIg."13 2 2 L1544 CH3OH

Fig.%14 LTE non-lte Bizzocchi 2 3 30m LTE non-lte (MONACO%code) 1 (fig.%14)

#27 Study&of&the&filamentary&infrared&dark&cloud&G192.76+00.10&in& the&s254>s258&ob&complex Introduction Andre& et&al 2014 D&=&1.78&+&0.12kpc S254>S258 G192.76&+&00.10 Fig.&1 H&II S254 S258 62 YSOs 1Myr YSOs (Klessen&et& al. 2004

Table&1 9.3&km&/&s Fig.&3 PV&diagrams&in&the&lines13CO(2 1)&(top),13CO(1 0)& (middle)&and&cs&(bottom). Fig.&2 13CO(150) 13CO 2 13CO 2kms51

Fig.%6 13CO(2B1) H2 Fig.%7 The%profiles%of%the%H2column%density morphology H2 fig.%6 main%filament mait 12 CO NH 3 10~35K S258%HII 5.1 10 22 cm B2 800Mo. 7pc 115Mo/%pc 1%pc 6 CS 2B1 30 160Mo 0.16 0.78

#19 Inside-Out'Planet'Formation.'IV.'Pebble'Evolution'and'Planet' Formation'Timescales Systems'with'tightly-packed'inner'planets'(STIPs)'are'very'common.'Chatterjee&Tan'proposed'Inside-Out' PlanetFormation'(IOPF),'anin'situformation'theory,'to'explain'these'planets.'IOPF'involves'sequential'planet' formationfrom'pebble-rich'rings'that'are'fed'from'the'outer'disk'and'trapped'at'the'pressure'maximum'associated'with' thedead'zone'inner'boundary'(dzib).'planet'masses'are'set'by'their'ability'to'open'a'gap'and'cause'the'dzib'to' retreatoutwards.'we'present'models'for'the'disk'density'and'temperature'structures'that'are'relevant'to'the'conditions' ofiopf.'for'a'wide'range'of'dzib'conditions,'we'evaluate'the'gap'opening'masses'of'planets'in'these'disks'that' areexpected'to'lead'to'truncation'of'pebble'accretion'onto'the'forming'planet.'we'then'consider'the'evolution'of' dustand'pebbles'in'the'disk,'estimating'that'pebbles'typically'grow'to'sizes'of'a'few'cm'during'their'radial'drift' fromseveral'tens'of'au'to'the'inner,< 1'AU-scale'disk.'A'large'fraction'of'the'accretion'flux'of'solids'is'expected'to'be' insuch'pebbles.'this'allows'us'to'estimate'the'timescales'for'individual'planet'formation'and'entire'planetary' systemformation'in'the'iopf'scenario.'we'find'that'to'produce'realistic'stips'within'reasonable'timescales'similar'to' disklifetimes'requires'disk'accretion'rates'of 10 9M yr 1and'relatively'low'viscosity'conditions'in'the'DZIB'region,i.e.,' Shakura-Sunyaev'parameter'ofα 10 4.

#20 The&Herschel8PACS&legacy&of&low8mass&protostars:&Properties&of& warm&and&hot&gas&and&its&origin&in&far8uv&illuminated&shocks Recent&observations&from&Herschel&allow&the&identification&of&important&mechanisms&responsible&for&the&heating&of& gassurrounding&low8mass&protostars&and&its&subsequent&cooling&in&the&far8infrared&(fir).&shocks&are&routinely&invokedto& reproduce&some&properties&of&the&far8ir&spectra,&but&standard&models&fail&to&reproduce&the&emission&from&keymolecules,& e.g.&h2o.&here,&we&present&the&herschel8pacs&far8ir&spectroscopy&of&90&embedded&low8mass&protostars(class&0/i).&the& Herschel8PACS&spectral&maps&covering 55 210μm&with&a&field8of8view&of 50PPare&used&to&quantifythe&gas&excitation& conditions&and&spatial&extent&using&rotational&transitions&of&h2o,&high8jco,&and&oh,&as&well&as&[oi]&and&[c&ii].&we&confirm& that&a&warm&( 300&K)&CO&reservoir&is&ubiquitous&and&that&a&hotter&component&(760 170K)&is&frequently&detected& around&protostars.&the&line&emission&is&extended&beyond 1000&AU&spatial&scales&in&40/90objects,&typically&in&molecular& tracers&in&class&0&and&atomic&tracers&in&class&i&objects.&high8velocity&emission&(> 90km&s 1)&is&detected&in&only&10& sources&in&the&[o&i]&line,&suggesting&that&the&bulk&of&[o&i]&arises&from&gas&that&is&movingslower&than&typical&jets.&line&flux& ratios&show&an&excellent&agreement&with&models&of&c8shocks&illuminated&by&uvphotons&for&pre8shock&densities& of 105cm 3and&UV&fields&0.1 10&times&the&interstellar&value.&The&far8IR&molecularand&atomic&lines&are&a&unique& diagnostic&of&feedback&from&uv&emission&and&shocks&in&envelopes&of&deeply&embeddedprotostars.

#22 Characterization)of)methanol)as)a)magnetic)field)tracer)in)star; forming)regions Magnetic)fields)play)an)important)role)during)star)formation.)Direct)magnetic)field)strength)observations)have) provenparticularly)challenging)in)the)extremely)dynamic)protostellar)phase.)because)of)their)occurrence)in)the)densest) partsof)star;forming)regions,)masers,)through)polarization)observations,)are)the)main)source)of)magnetic)field) strengthand)morphology)measurements)around)protostars.)of)all)maser)species,)methanol)is)one)of)the)strongest)and) mostabundant)tracers)of)gas)around)high;mass)protostellar)disks)and)in)outflows.)however,)as)experimental) determinationof)the)magnetic)characteristics)of)methanol)has)remained)largely)unsuccessful,)a)robust)magnetic)field) strength)analysisof)these)regions)could)hitherto)not)be)performed.)here,)we)report)a)quantitative)theoretical)model)of) the)magneticproperties)of)methanol,)including)the)complicated)hyperfine)structure)that)results)from)its)internal) rotation.)we)showthat)the)large)range)in)values)of)the)land)g)factors)of)the)hyperfine)components)of)each)maser)line) lead)to)conclusionsthat)differ)substantially)from)the)current)interpretation)based)on)a)single)effective)g)factor.)these) conclusions)aremore)consistent)with)other)observations)and)confirm)the)presence)of)dynamically)important)magnetic) fields)aroundprotostars.)additionally,)our)calculations)show)that)(nonlinear))zeeman)effects)must)be)taken)into)account) to)furtherenhance)the)accuracy)of)cosmological)electron;to;proton)mass)ratio)determinations)using)methanol.

#23 NearAinfrared#study#of#new#embedded#clusters#in#the#Carina# complex We#analyse#the#nature#of#a#sample#of#stellar#overdensities#that#we#found#projected#on#the#Carina#complex.#This#studyis# based#on#2mass#photometry#and#involves#the#photometry#decontamination#of#field#stars,#elaboration#of#intrinsiccoloura magnitude#diagramsj (J Ks),#colourAcolour#diagrams#(J H) (H Ks)#and#radial#density#profiles,#inorder#to#determine# the#structure#and#the#main#astrophysical#parameters#of#the#best#candidates.#the#verification#ofan#overdensity#as#an# embedded#cluster#requires#a#cmd#consistent#with#a#pms#content#and#ms#stars,#if#any.#fromthese#results,#we#are#able#to# verify#if#they#are,#in#fact,#embedded#clusters.#the#results#were,#in#general,#rewarding:in#a#sample#of#101#overdensities,# the#analysis#provided#15#candidates,#of#which#three#were#previously#catalogued#asclusters#(cccpacl16,#treasure#chest# and#fsr1555),#and#the#12#remaining#are#discoveries#that#provided#significantresults,#with#ages#not#above#4.5myr#and# distances#compatible#with#the#studied#complex.#the#resulting#values#for#thedifferential#reddening#of#most#candidates# were#relatively#high,#confirming#that#these#clusters#are#still#(partially#or#fully)embedded#in#the#surrounding#gas#and#dust,# as#a#rule#within#a#shell.#histograms#with#the#distribution#of#the#masses,ages#and#distances#were#also#produced,#to#give# an#overview#of#the#results.#we#conclude#that#all#the#12#newly#foundembedded#clusters#are#related#to#the#carina# complex.

#24 The#physical#and#chemical#structure#of#Sagittarius#B2.#III.# Radiative#transfer#simulations#of#the#hot#core#SgrB2(M)#for# methyl#cyanide We#model#the#emission#of#methyl#cyanide#(CH3CN)#lines#towards#the#massive#hot#molecular#core#SgrB2(M).#Weaim#at# reconstructing#the#ch3cn#abundance#field#and#investigating#the#gas#temperature#distribution#as#well#as#thevelocity#field.# SgrB2(M)#was#observed#with#the#ALMA#in#a#spectral#line#survey#from#211#to#275#GHz.#This#frequencyrange#includes# several#transitions#of#ch3cn#(including#isotopologues#and#vibrationally#excited#states).#we#employ#thethreem dimensional#radiative#transfer#toolbox#pandora#in#order#to#retrieve#the#velocity#and#abundance#field#by# modelingdifferent#ch3cn#lines.#for#this#purpose,#we#base#our#model#on#the#results#of#a#previous#study#that#determined# thephysical#structure#of#sgrb2(m),#i.e.#the#distribution#of#dust#dense#cores,#ionized#regions#and#heating#sources.# Themorphology#of#the#CH3CN#emission#can#be#reproduced#by#a#molecular#density#field#that#consists#of#a# superpositionof#cores#with#modified#plummermlike#density#profiles.#the#averaged#relative#abundance#of#ch3cn#with# respect#to#h2ranges#from#4 10 11to#2 10 8in#the#northern#part#of#SgrB2(M)#and#from#2 10 10to#5 10 7in#the# southern#part.in#general,#we#find#that#the#relative#abundance#of#ch3cn#is#lower#at#the#center#of#the#very#dense#and#hot# cores,#causingthe#general#morphology#of#the#ch3cn#emission#to#be#shifted#with#respect#to#the#dust#continuum#emission.# The#dusttemperature#calculated#by#the#radiative#transfer#simulation#based#on#the#available#luminosity#reaches#values#up# to#900k.#however,#in#some#regions#vibrationally#excited#transitions#of#ch3cn#are#underestimated#by#the#model,# indicatingthat#the#predicted#gas#temperature,#which#is#assumed#to#be#equal#to#the#dust#temperature,#is#partly# underestimated.the#determination#of#the#velocity#component#along#the#line#of#sight#reveals#that#a#velocity#gradient# from#the#north#tothe#south#exists#in#sgrb2(m).

#26 Spiral'density'waves'and'vertical'circulation'in'protoplanetary' discs Spiral'density'waves'dominate'several'facets'of'accretion'disc'dynamics' planet5disc'interactions'and' gravitationalinstability'(gi)'most'prominently.'though'they'have'been'examined'thoroughly'in'two5dimensional' simulations,their'vertical'structures'in'the'non5linear'regime'are'somewhat'unexplored.'this'neglect'is'unwarranted' given'thatany'strong'vertical'motions'associated'with'these'waves'could'profoundly'impact'dust'dynamics,'dust' sedimentation,planet'formation,'and'the'emissivity'of'the'disc'surface.'in'this'paper'we'combine'linear'calculations'and' shearingbox'simulations'in'order'to'investigate'the'vertical'structure'of'spiral'waves'for'various'polytropic'stratifications andwave'amplitudes.'for'sub5adiabatic'profiles'we'find'that'spiral'waves'develop'a'pair'of'counter5rotating'poloidalrolls.' Particularly'strong'in'the'nonlinear'regime,'these'vortical'structures'issue'from'the'baroclinicity'supported'bythe' background'vertical'entropy'gradient.'they'are'also'intimately'connected'to'the'disk s'g5modes'which'appearto'interact' nonlinearly'with'the'density'waves.'furthermore,'we'demonstrate'that'the'poloidal'rolls'are'ubiquitousin' gravitoturbulence,'emerging'in'the'vicinity'of'gi'spiral'wakes,'and'potentially'transporting'grains'offthe'diskmidplane.' Other'than'hindering'sedimentation'and'planet'formation,'this'phenomena'may'bear'on'observations'ofthe'disk s' scattered'infrared'luminosity.'the'vortical'features'could'also'impact'on'the'turbulent'dynamo'operatingin'young' protoplanetary'discs'subject'to'gi,'or'possibly'even'galactic'discs.

#28 Orbital#Motion#of#Young#Binaries#in#Ophiuchus#and#Upper# Centaurus<Lupus We#present#measurements#of#the#orbital#positions#and#flux#ratios#of#17#binary#and#triple#systems#in#the#Ophiuchus# starforming#region#and#the#upper#centaurus<lupus#cluster#based#on#adaptive#optics#imaging#at#the#keck#observatory.# Wereport#the#detection#of#visual#companions#in#MML#50#and#MML#53#for#the#first#time,#as#well#as#the#possible# detectionof#a#third#component#in#wsb#21.#for#six#systems#in#our#sample,#our#measurements#provide#a#second#orbital# positionfollowing#their#initial#discoveries#over#a#decade#ago.#for#eight#systems#with#sufficient#orbital#coverage,#we# analyze#therange#of#orbital#solutions#that#fit#the#data.#ultimately,#these#observations#will#help#provide#the#groundwork# towardmeasuring#precise#masses#for#these#pre<main#sequence#stars#and#understanding#the#distribution#of#orbital# parametersin#young#multiple#systems.