SFN$306$No.55+60$
2018/07/20
 
55. Chandra$Detection$of$An$Evolved$Population$of$Young$Stars$in$Serpens$South$
56. Extended$ammonia$observations$towards$the$‘Integral+Shaped$Filament’$
57. CO$in$Protostars$(COPS):$Herschel+SPIRE$Spectroscopy$of$Embedded$Protostars$
58. Stellar$masses$and$disk$properties$of$Lupus$young$stellar$objects$traced$by$velocity+aligned$stacked$ALMA$13CO$and$C18O$spectra
59. Complex$organic$molecules$in$the$Galactic$Centre:$the$N+bearing$family
60. Planet$Formation$in$Highly$Inclined$Binary$Systems.$II.$Orbital$Alignment$or$Anti+alignment$and$Planet$Growth$Boost$in$Intermediate$Separation$Binaries$

#56

Extended'ammonia'observa0ons'towards'the'‘Integral7Shaped'
Filament’'

Gang'Wu1,'2,'3,'4,'Keping'Qiu2,'Jarken'Esimbek1,'3,'Xingwu'Zheng2,'Christian'Henkel5,'6,'Dalei'Li1,'and'
XiaoHong'Han1'

hPp://arxiv.org/pdf/1805.11242'

Introduction• #Ei>,46ejTz~-'FZRhH^v\fZ!tYh]w
dWv(e.g.,'André'et'al.'2010;'Jackson'et'al.'2010;'Li'et'al.'2014)• >hswkTz~h)baIjTnoiOQthe'“sausage”'
instability'(e.g.,'Jackson'et'al.'2010)e=twvj_U• z~jTRiffragmentationx@mTBN"i &(Px?^v$%gU• ‘integral7shaped'filament’'(ISF)jTcometary-Orion'A cloudi 7hVvcompact'ridge• ISFhjTOMC71TOMC72TOMC73TOMC74TXslOMC75iW[cYiclumpZpwT ISFj*1gBN"|{~eTI
2iOh0gvi":Z.pwT2ri<W"ZpwdWvU• yyNH3i DK5jTdepletionZVpug[T`iC9'FTXsl
G +h^viaqhTAMg3}e^U• NH31,1Xsl2,2i;/j8103cm73eVuTz~iSLf`wtifragmentationiaqiJg~ |NH3(1,1)((((((((((((((((((((NH3 (2,2)

Fig.(1• NH3)morphology* 768'
!%2integral7shaped(filament(4"• OMC74) ( ! 3#2(PC)sub7filament0NH3&/% Fig.(2••••6$)clumps'11)sub7clumps
culmp*",%-.
1.36(pc'sub(*0.86(pc )56)1+
fragmentaGon'Discussion
velocity.map

averaged.centroid.velocity.diagram
13CO
NH3

Fig..6Fig..3.(left.panel)• ISFJEF0.6.km11 pc11K/ 17:CS>[`[bAK #I+KDP7• ?K/X"9F6ISFK+Z_a]cH2 Z_a]cX,ADH?WL%
0.25G8T6+Z_a]cL2 Z_a]cKNYK07• ISFJED2/X(Fig..6)•  LISFJEF)SVOB7 OMC115LBMF6 K'.J&7?V
L6\^<ISFKcumpJ ;EF VU?HX$AF9U;QAVI9<6J3AFQ*BU?H<G=U7• OMC11-K13COJBUNH3K5(I/jump!NH3Lhot.dense.clumpJREFenhance@VF:T613COLJ6!\^J4AF9U7(1)rotation6temperature

Fig.67• OMC$1- .30$40K"• ISF-$1/+13# 620K7& "• OMC$2!OMC$3!$1/OMC$4-.!(42-clump- +13& '!
+13#5)"!&, %2(3!(42-clump&0*-- #58

Stellar'masses'and'disk'proper0es'of'Lupus'young'stellar'objects'
traced'by'velocity:aligned'stacked'ALMA'13CO'and'C18O'spectra'

Hsi:Wei'Yen1,'Patrick'M.'Koch2,'Carlo'F.'Manara1,'Anna'Miotello1,3'and'Leonardo'Testi

hMps://arxiv.org/pdf/1804.06272.pdf'

3PALMA_qj\KQ; ($P AP_pio@, CZJ=Y@9=S'/'NKQM=<%'KQ;2)fqc?X5 >WRdisk![.SYHU;velocity:aligned'
stacking'method'["=Y<Method• LupusP88PYSOPALMA'13COr3:2s>WRC18Or3:2sfqc["=H<• CZH^inq4[VLN;diskP#MY*Kak]go[CFH;GZX[&T6OY<• ^inq 0P4hcqpQ4IPhnmqcK+CZY(/7(M:) ;81P*-rPAs;-ris;`ael4rVsyss• acd]CZHak]goPS/N[ NEYhnmqcbdg[D; LDJBPhnmqc
bdg["=H<Fig.'1

• 18EdsikA13COQ=118EdiskAC18O
Q2• RY,Lup1J16083070438282686LHSz,83Edisk,
orientationQ"2• P4V7MM01PA1i1VsysQJ>• UVWR]S!DLOF1(7<E* A&$7ME"B+Fig.,2• =>13COEdiskE23F1conDnuum7MPABi8"<P@5O^Ansdell,et,al212016;,Tazzari,et,al212017_2• 3E!7M<P>PAFconDnuum7MEKEB'/• diskEinclinaDonK'/=@5O81LN9CGM?984O• !F1disk,orientaDonQ#)DA91conDnuumI>FlineE(C8C5 AKM7DCO2Fig.,4Fig.,11• =>13COEdiskE37FE,.8E- [X\A %D <P@5O• <P> %,.F1 ,.B+=@
6N12?E,.EF0.15Mo2• ;ETYT]Z\E %,.F1 0.1Mo7M2Mo
IAE,.* E[X\BL:+2

Fig.%12Fig.%13•  BYEdiskNtotal%gas-2Z8!BYE13CO<UQC18ONZdisk%model (Williams%&%Best,%2014)K .D
XAKMUGI9• 13CO,%C18O=V+(TVYX7;disk%gas-2O8
con?nuumJ+(TVYX7;disk%dust-2K5CI;
X >:W8)4Z'9[\ A ]\^ O8disk%
dust-2MCL;AKZ'D9• disk%gas<UQdust%-2N O?LPVH?>:W8gas%A dust-2 O834N>:X9• 0 N1*L"$<UQ >#Ndisk-2+(TWMORFL@8BYXdisk%gas-2N&BZT
EVCI;X9• viscously%evolving%disksN$,M<;I8 mass%accre?on%
rateKdisk%total%massKN3N%4N>!BYX9• C=C8mass%accre?on%rate%K13COKC18O=V+(TVY
Xdisk%gas%massKN3ML%4O+VYL;9• disk%gas-2Kdisk%dust-2KN%4>:GIT813CO=
VNtotal%gass-2Z DX6N?LNES
M8 mass%accre?on%rateKdisk%total%massKN%4O+/R
YL;

#59

Complex(organic(molecules(in(the(Galac4c(Centre:(the(N7bearing(familyZeng1,(I.(Jim(́enez7Serra1,(V.(M.(Rivilla2,(S.(Mart(́ın3,4,(J.(Mart(́ın7Pintado5,(M.(A.(Requena7Torres6,(J.(Armijos7Abenda7,(D.(Riquelme8(and(R.(Aladro

https://arxiv.org/pdf/1804.11321(Introduction• 0e^aJ6200b S#D^& Vk]NjSJYb63 b1Scomplex(organic(molecules(|COM}^Mj_9Phk]NjK(mrszpursw{^cJCOMc:aJ6
bl$Xj.7$ )• (L`#D1aQN]JCOMcahot(coreaEAW]Nj_9Phk]NjK• YbJcold(dark(cloud(core,(molecular(ou_low,(prestellar(core,(PDR^f&• COMb2 ",ci) CH3OHeZcH2CObgO` H/>Rhb*4ag[]T`COMSii) dust(grain;Gb+7eZcvqnxvqnxWJ*4a! Vkj• Galac4c(Centre(quiescent(giant(molecular(cloud((QGMC)cJ'5`%^COMb
8?lgigU FXj• 50K~120KbINorB-J30KbNdust-J)@3NH2or~104cm73• G+0.69370.027|G+0.693}cJCbGC hot(core(SgrB2|N}a<hkjgO`ytxb
3=Qgd(l$XjGC(QGMCb1\• GBT*(IRAM(30m , "Galactic(Centre(quiescent(giant(molecular(cloud((QGMC),(G+0.693% "unbiased(spectral(line(survey• N%+ &%!") $ ,)+
• N%+ #17& clear(detecJons(and(2(&tentaJve(detecJons• &8 'complex(organic(molecules-COM.#+Fig.(2Fig.(1• H2|#rx10+11l10+8}_$|dh[AsFig.%4• G%+%0.693yO;qt hHC5NHC7N6~e\:)|koF =}(} | H+
• G%+%0.693y~eb CH3NH2~bCH2NH U"|Njmehot%corey~5 #ygfhot%core eG+0.693}/m  =?{8E m-3qxh• bC2H3CNmbC2H5CN|6xU"|spzR0s1H+}g~eF}(| vxYq 7@ • G%+%0.693k shock`L1157+B1jCH3CNeHC5NeHNCOk NH2CHOy;qt ]}aJ{ImNqfp~e%C}Xshock|khxedustl}9}Z mgrain%spuOeringrx7@|.qtzhiGj(Sf• G+0.693%~L^{NU"|eCentral%Molecular%Zone%(CMZ,%the%central%500pc%of%the%Milky%Way)}1}24 BVK'}1w• G%+%0.693uoy{n\:DyCOMs}W<q|St|~e dh,&z dhP& QHe n} c! cz>Tm*M

#55

Chandra#DetecXon#of#An#Evolved#PopulaXon#of#Young#Stars#in#
Serpens#South

We#present#a#Chandra#study#of#the#deeply#embedded#Serpens#South#star5forming#region,#examining#cluster#structure#
and#disk#properties#at#the#earliest#stages.#In#total,#152#X5ray#sources#are#detected.#Combined#with#Spitzer#and#2MASS#
photometry,#66#X5ray#sources#are#reliably#matched#to#an#IR#counterpart.#We#identify#21#class#I,#6#flat#spectrum,#16#class#II,#
and#18#class#III#young#stars;#5#were#unclassified.#Eighteen#sources#were#variable#in#X5rays,#8#exhibiting#flare5 like#emission,#
and#one#periodic#source.#The#cluster#X5ray#luminosity#distance#was#estimated,#the#best#match#was#to#the#nearer#distance#of#260#pc#for#the#front#of#the#Aquila#Rift#complex.#The#NH#vs.#AK#ratio#is#found#to#be#∼0.68# 1022,#similar#to#that#measured#in#other#young#low#mass#regions,#but#lower#than#that#measured#in#the#ISM#and#high#mass#clusters#(∼(1.6–2)#
 1022).#We#find#the#spatial#distribution#closely#follows#that#of#the#dense#filament#from#which#the#stars#have#formed,#
with#the#class#II#population#still#strongly#associated#with#the#filament.#There#are#four#sub5clusters#in#the#field,#with#three#forming#knots#in#the#filament,#and#a#fourth#to#the#west,#which#may#not#be#associated#but#may#be#contributing#to#the#
distributed#class#III#population.#A#high#percentage#of#diskless#class#IIIs#(upper#limit#30%#of#classified#X5ray#sources)#in#such#a#young#cluster#could#indicate#that#processing#of#disks#is#influenced#by#the#cluster#environment#and#is#not#solely#
time5scale#dependent.#

#57

CO#in#Protostars#(COPS):#Herschel@SPIRE#Spectroscopy#of#
Embedded#Protostars#

We#present#full#spectral#scans#from#200–670#μm#of#26#Class#0+I#protostellar#sources,#obtained#with#Herschel@SPIRE,#as#
part#of#the#”COPS@SPIRE”#Open#Time#program,#complementary#to#the#DIGIT#and#WISH#Key#programs.#Based#on#our#nearly#conOnuous,#line@free#spectra#from#200–670#μm,#the#calculated#bolometric#luminosiOes#(Lbol)#increase#by#50%#on#
average,#and#the#bolometric#temperatures#(Tbol)#decrease#by#10%#on#average,#in#comparison#with#the#measurements#
without#Herschel.#FiXeen#protostars#have#the#same#Class#using#Tbol#and#Lbol/Lsmm.#We#idenOfy#rotaOonal#transiOons#of#
CO#lines#from#J#=#4#→#3#to#J#=#13#→#12,#along#with#emission#lines#of#13CO,#HCO+,#H2O,#and#[C#i].#The#raOos#of#12CO#to#
13CO#indicate#that#12CO#emission#remains#opOcally#thick#for#Jup#<#13.#We#ﬁt#up#to#four#components#of#temperature#
from#the#rotaOonal#diagram#with#ﬂexible#break#points#to#separate#the#components.#The#distribuOon#of#rotaOonal#
temperatures#shows#a#primary#populaOon#around#100#K#with#a#secondary#populaOon#at#∼350#K.#We#quanOfy#the#correlaOons#of#each#line#pair#found#in#our#dataset,#and#ﬁnd#the#strength#of#correlaOon#of#CO#lines#decreases#as#the#
diﬀerence#between#J@level#between#two#CO#lines#increases.#The#mulOple#origins#of#CO#emission#previously#revealed#by#
velocity@resolved#proﬁles#are#consistent#with#this#smooth#distribuOon#if#each#physical#component#contributes#to#a#wide#
range#of#CO#lines#with#signiﬁcant#overlap#in#the#CO#ladder.#We#invesOgate#the#spaOal#extent#of#CO#emission#and#ﬁnd#that#the#morphology#is#more#centrally#peaked#and#less#bipolar#at#high@J#lines.#We#ﬁnd#the#CO#emission#observed#with#SPIRE#
related#to#ouhlows,#which#consists#two#components,#the#entrained#gas#and#shocked#gas,#as#revealed#by#our#rotaOonal#
diagram#analysis#as#well#as#the#studies#with#velocity@resolved#CO#emission.#

#60

Planet&FormaQon&in&Highly&Inclined&Binary&Systems.&II.&Orbital&Alignment&or&AnQG alignment&and&Planet&Growth&Boost&in&
Intermediate&SeparaQon&Binaries

Stars&are&commonly&formed&in&binary&systems,&which&provide&a&natural&laboratory&for&studying&planet&formation&in&extreme&conditions.&In&our&first&paper&(Paper&I)&of&a&series&(Xie&et&al.&2011),&we&have&shown&that&the&intermediate&stage&— from&planetesimals&to&planetary&embryos/cores&— of&planet&formation&can&proceed&even&in&highly&inclined&binaries.&
Following&Paper&I,&here&we&numerically&study&the&late&stage&of&terrestrial&planet&formation,&i.e.,&from&embryos&to&full&planets,&in&binary&systems&of&various&orbital&configurations.&We&identify&an&orbital&alignment&or&antiGalignment&effect;&
namely,&although&an&inclined&binary&generally&misaligns&the&planetary&orbits&with&respect&to&the&spin&axis&of&the&primary&host&star&(i.e.,&causing&large&obliquity),&it&could&align&or&antiGalign&the&planetary&orbits&with&respect&to&the&binary&orbit.&Such&an&orbital&(antiG)alignment&effect&is&caused&by&the&combination&of&orbital&differential&precession&and&selfGdamping,&
and&it&is&mostly&significant&in&cases&of&intermediate&binary&separations,&i.e.,&aB&∼ 40–200&AU&for&terrestrial&planet&formation&around&1&AU&from&the&primary&stars.&In&such&intermediate&separation&binaries,&somewhat&contrary&to&intuition,&
the&binary&companion&can&aid&planet&growth&by&having&increased&the&rate&of&collisions,&forming&significantly&more&massive&but&fewer&planets.&In&the&other&two&ends,&the&companion&is&ether&too&close&thus&plays&a&violently&disruptive&role&or&too&wide&to&have&significant&effect&on&planet&formation.&Future&observations,&which&can&discover&more&planetGbearing&binary&star&systems&and&constrain&their&masses&and&3GD&orbital&motions&will&test&our&numerical&findings.&