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$OB$
complex28. 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%• ^aZYH*"E Q&,@PAKG8WRHQ@P>E=1*
D:P9• ALMAI8mm%DH[Y]H0(%GMBC8WRQ J6HTY$/Q @PAKG4G 9• ALMAQ'?C8Fc105Mod.) 73cIRDCdG28.37%+%0.07H5H6TYEWRH-#• 12m arrayH86_Sb\SbVH`XSU<NFO8>HIRDCH!LF$/HHF;+2Q• MIREXC1ALMAUMJK0 >Σ>0.2-g-cm122• Spitzer-IRAC-8μmBdark-regionA• MIREXTPSC1ONQYΣAZADF#I%91ALMACONQYΣ?ONQ!
AZ•TPSCIQVXN91ALMA+&C1LWRKQ>1>54*1:@H< >3F?8GF*I$
A%:2•,Bpre1stellar-core-?47=5Bmassivepre1stellar-core61ALMA+&>A
8G>4F
FIg. 1 :MIREXTPS5EB.B(-/?ALMA>'"8G;1.3-mmBONQ+&?B)
Contours:-ALMA-1.3-mm-continuum-mosaic.
The-two-red-contours-highlight-SNR-=-3-and-10.

Fig.%2• Σ& %ALMA1.3%mm&01/,.*!( $(• / &-+*! )'-+/IRDC&Σ"!(  #*!

Fig.%4• * RgV1.3mm^C8-wzpmo_G`a \protostellar-CMFiLG pre1stellar-CMFNd^ib9!_/>Uf[Uf[&#nj 1_fdgT• ,]GI^njNd^&# 1Ojlsw~wktupm^yr|]XKY
"Rgf650ZJf[Uf[G2?RgYKfnjNd#Rgf&^AE_fdg^6 GU\hWε*58H• * RgV1.3mm+BO]protostellar-coresis}oSGnj^AE^D i%$Uf[SYGQgd^7)iIRDC]MPf&# 1G0]:4;'FJVe^&# 1εffi=5cf• Q^@(Z_GMcKeeTan2003^.njyr|i 3SYGnj^x~vqki^mzx^x~vqk[{mUfyr|O <ZGI^&#'F_GSYGmzx^:4;'F^6 H• "Rgfnj 1 &# 1(εcore)O650^Gεff≃fdg≃10[=5cdgf

#25 Seeds%of%Life%in%Space%(SOLIS).%III.%Zooming%into%the%methanol%peak%of%the%pre;stellar%core%L1544

Introduction••••SJNXU(CH3OH)76'6186%!4 $&QVMIJX =6DWRVXQ:*( 6cold%dense%cloudsA/SJNXU7*CO( 62#2+>3.?>L15447 4pre;stellar%core(n~2x10^6%cm^;3)
Observation• NOEMA"• beam%:5.71”x3.86”• 20”;=9 -4IGXU,<6A
EOX/>185*SJNXUTCW6IRAM%30mANOEMALXJ3@01• SJNXU(CH3OH)7KIMPXF65

Fig.%1color%scale%:CH3OHIRAM%30m)HWMB250%µm%dust%continuumResultsFig.22
The2white2contours2:21.22mm2dust2continuum2emission
The2yellow2cross2shows2the2dust2emission2peak.

Fig.23

NOEMA+30m

NOEMA.(+20&#  ! (FIg.2)• NOEMA+30m&1,%*$-)'/1 (Fig.23)•  ! "•

Results

Fig."13Fig."4Fig."7

Velocity"dispersions"of"theA+methanol"line.

• 5?U8 9B07"km"s&1"pc&1W-U8 <(Fig."7)•VFPR8G(Fig."4)• HU8XApre&stellar"coreW /VFPR>LAfjGhdV]PI`
T=,NaJTV^PR(KbRDa 3• W 3XA7!UHerschelljo:2"tms|FIg."13}V6_ba2QWZ[+UrewuzoW4.V^PR(Ma;@8ivmgSC`A2QW%VL1544u
kp{xq{gG6_baB• LFLUG_A') 3Uukp{xn{kXAEYCH3OHV^PRoy{jKbafjW#c$NaJTGSHUDO\AJWSW4Wc1*
V&NaWVX SCaB

Fig.%14• LTEdPT91PR^YVGnon-LTEvlxd.JT91PRujo{x#ZG;
 U5QbKGkimq{gX?J#ZGBizzocchi`X_bE8+U(]`cR#Y23 H NcZG")PRujo{xYB dB /XCQbL
W30mYp{tX_ST<!QbNVKULbH• =*Y91ZGujo{xK6PM%PRkimq{g?Y\ujo{xKLTEX?JNVd0PTJbH• non-LTE &syrefxdGvlxPR(MONACO%code)ujo{x&syrefxV&>PQbVGsyrefxZvlx+V5PTJbKG1$J
D(fig.%14)H• vlxU .OcTJb4F ,[RZ'2mznwzhY ,KA:OcTJb3KIb• ujo{xYDd_a_M -QbR]XZ@vlxK7

#27

Study&of&the&filamentary&infrared&dark&cloud&G192.76+00.10&in&
the&S254>S258&OB&complex

Introduction•5P')Q?<C\Z^]_["P6YJKAWEMY(GKAW`Andre&et&al@?2014a• D&=&1.78&+&0.12kpcP4;L. S254>S258O+HW\Z^]_["3*<G192.76&+&00.10Y')HW

Fig.&1• 8Q?H&II=S254S258
OTJK0$FXKAW@• \Z^]_[O JKGKAW62
PYSOsC G?EP=Q1MyrTV
S,A@:-CBIUDEP<P
PYSOsP9%N(Klessen&et&al. 2004a• &%Q?EP<P7?IP-M!
#%2Y O>A/L1R
WEM

Table&1• 7*J/ 3• ]Wa`cZ0M89.3&km&/&sL/HO
Q@+RUTFig.&3 PV&diagrams&in&the&lines13CO(2–1)&(top),13CO(1–0)&(middle)&and&CS&(bottom).

Fig.&2 13CO(150)• [YK ED.(L,V+TI
LOL9• '-K ED)P=J/ 3>ME?SI+RUT9• 2HM8#K13COK<;G8QS;/HL&2L/ >+RUT9• 13COY_XZbLM85KAAH
4K\dXK1BG;TAIV%BG;NC9• ;@F=LXac^K
CTAI>H?NC9•
.(L(M2kms51H:S8AUM"$V?@S86 L7*J!VCT9

Fig.%7Fig.%6The%profiles%of%the%H2column%density

13CO(2B1)Si-f[H2*$• morphologydH2*$}v{ fig.%6b>ilkhQbMSaj=IN main%filamentb R^Mmait` Y31Y^Pk;&cOkM)Cb$czow0+ATZk• 12CO`NH3Si-filkqt/$d10~35KNS258%HIIJbS\^• ,8p~$dM5.1L1022 cmB2Nzowc9?Ed7800Mo._OjMFXd
77pc_OkN:?Ed115Mo/%pc_OjMWld<2hjgKVM 4
TYaPcD &m5ZN• qt*$ !Si%ilkzowc#"d71%pc_OjM(Gzowc#hjgdkSbUPNWldM@ c. cs|wbHBY^Pk;&TOjeZN• 6]cK$r{TCS 2B1_XlM?Ed30160Moc6 bOjMy
nxucd0.160.78c6_OjMD &m'ZkN

#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&(760170K)&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#410−11to#210−8in#the#northern#part#of#SgrB2(M)#and#from#210−10to#510−7in#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.