SFN$310$No.10*18$
2018/11/9
 
10. The$Ophiuchus$DIsc$Survey$Employing$ALMA$(ODISEA)$* I$:$project$description$and$
continuum$images$at$28$au$resolution
11. High$resolution$millimetre$imaging$of$the$CI$Tau$protoplanetary$disc$— a$massive$
ensemble$of$protoplanets$from$0.1–100$au$
12. Magnetically$induced$termination$of$giant$planet$formation$$
13. Simultaneous$spectral$energy$distribution$and$near*infrared$interferometry$modeling$of$
HD$142666$
14. THE$STUDY$OF$A$SYSTEM$OF$HII$REGIONS$TOWARD$L$=$24 .8,$B$=$0 .1$AT$THE$GALACTIC$
BAR$* NORMA$ARM$INTERFACE$
15. Multiple$Disk$Gaps$and$Rings$Generated$by$a$Single$Super*Earth:$II.$Spacings,$Depths,$and$Number$of$Gaps,$with$Application$to$Real$Systems$
16. Clumpy$shocks$as$the$driver$of$velocity$dispersion$in$molecular$clouds:$the$effects$of$self*
gravity$and$magnetic$fields
17. The$Gaia$DR2$view$of$the$Gamma$Velorum$cluster:$resolving$the$6D$structure
18. Synthetic$[CII]$emission$maps$of$a$simulated$molecular$cloud$in$formation$#14 THE$STUDY$OF$A$SYSTEM$OF$HII$REGIONS$TOWARD$L$=$24 .8,$B$=$

0 .1$AT$THE$GALACTIC$BAR$= NORMA$ARM$INTERFACE$
L.$K.$Dewangan1,$J.$S.$Dhanya2,$D.$K.$Ojha3,$and$I.$Zinchenko$• O2 &MIR;<A/$Hii*9B6
l$=24~34

https://arxiv.org/pdf/1809.01599.pdf$

458?*2,0$-)

• !&*HII• MIR$bubbles$(N32,$N33,$N34,$N35,$N36)$

Fig.$1

N364&*HII"1#1*HII+O$star).%'/1'0HII*tdyn +0.4$= 1.3$Myr$
6.7GHz@6:BA@B3B 3&*H$II) • N36Cd$=$6.0kpcD+ the$bar=arm$interface)
• Herschel >7=(+HII$region+2330K• 27*ATLASGAL$dust$clumps


Fig.$4+• Spitzer%color0color%125%embedded%
protostars

Fig.%11dust%emission,%molecular%gas,%and%ionized%emission N36O  "• 109%km/s113%km/s2GMC
  • 4012km/s! Fig.%8Fig.%9

FIg.#12

Fig.#10• ∼33.3#pc#84 Keyhole#and#Key-$7fit1;• 228%8!AIH4)#
8-,:JHII&,#6.7GHzEBCIFEI>I,#embetted#cluster)• N367+.;the#barAarm#interface48the#cloudAcloud#collision(CCC)DG@?
=*• 7 0345(8"41;5)8 92.7A8.2Myr5
• /<9HII&8 '50) 86
=

#16 Clumpy'shocks'as'the'driver'of'velocity'dispersion'in'molecular'
clouds:'the'effects'of'self7gravity'and'magnetic'fields'

D.'H.'Forgan1⋆,'I.'A.'Bonnell

https://arxiv.org/pdf/1809.06601'• E% CD ?>-F2RZUPM,?>P[]WE*E,.<K9BDJ?@I:LK• 9LHAE!$F29EYNVTX72-BSQ^\_E0D):L
KLarson'relation (σ'∝ LΓ'with'Γ'≈'0.5'`MA8K9BM#;@4>72'
/ B"E1F&:LC6?>3• smoothed'particle'magnetohydrodynamics (SPMHD)M(42'/ B"
EARZUPM;@clumpyEOSM,.:=K3• RZUPE:5JG +"E/ M :=K
Initial'Conditions

AHC@GJKE&z;545!

Fig.#2

Fig.#5

Fig.#1• ,916DBE2"Γ=#0.3'1.26 6>/σ#' L6 &+=-#• Γ7" ?B6FI@ 3AHC@GJKE36 %:8AHC@
5 (#• .1"Γ≈0.56><*37+=1$4$&"&4$ 2" 
3+6powerlow> 2'<30)<#• $ -B*Cy,%z(>Γ7• NQPL ;=J?+F• " B5GD
geometryA)!.
• " C2%7)!4 ABE• "AGI2 8@OMSR>B+
K<J:?7>8J3• σ%2 L0B'7clumpy%
shockB 2 !@Larson%
relation6HB,#C2 /A59JNQPLB;?
&K1<JFig.%6Fig.%7

#10

The$Ophiuchus$DIsc$Survey$Employing$ALMA$(ODISEA)$< I$:$
project$description$and$continuum$images$at$28$au$resolution
http://arxiv.org/pdf/1809.08844

Lucas$A.$Cieza$et$al.

• !"CO #Ophiuchus$Molecular$Cloud$300%
Spitzer<selected$protoplanetary$discs (ODISEA)•  147$target(sample$A)1.3$mm$continuum$images$ (0.2PP,$28$au)• 11$binary$systems$ 1$triple$system133  • 27$
(with$4<σ$upper$limits$of$∼1.0$mJy),• stacking dust$mass$∼0.1$M⊕

Fig.$2
Fig.$1

Fig.%8  )%(&F1.3mm%<10mJy, FWHM%<0.2%"~28au
50%mJy,%100%mJy!")%(&147',*+15-~5largest%cavity% two%gaps Elias2F27

Fig.%9• 53  #8substructures%(inner%cavities,%rings,%gaps,%and/or%spiral%arms)• 4substructures%(radial%profile )• >%50mJysource 50-.11/21/ 
substructure$ Fig.%12• AKDIdisk<71CI%!S AQIH
G][_(Mdust >%0.5%M⊕)• '50(ZcabI1/3)JW[! H+G10M⊕YTS AQIH
G][_• ?RJ1&!I$3E=(• ^U[XZV\I J7Yc`X_^U[XH=/M>PRD9Q8• "N=# @RB^U[XI J<%15 au7^U[XI23e15dfJ <>%30au8• OphiuchusH;>Q][_I-0 J7
TaurusELupusIO:GI)9e1>2%Myrf
E2HO=D9Q• 6<59LF4*G. <,PRQ

Fig.%13

#11 High#resolution#millimetre#imaging#of#the#CI#Tau#protoplanetary#disc#— a#massive#ensemble#of#protoplanets#from#0.1–100#au#
We#present#high#resolution#millimeter#continuum#imaging#of#the#disc#surrounding#the#young#star#CI#Tau,#a#system#hosting#the#first#hot#Jupiter#candidate#in#a#protoplanetary#disc#system.#
The#system#has#extended#mm#emission#on#which#are#superposed#three#prominent#annular#
gaps#at#radii#∼13,#39#and#100#au.#We#argue#that#these#gaps#are#most#likely#to#be#generated#by#
massive#planets#so#that,#including#the#hot#Jupiter,#the#system#contains#four#gas#giant#planets#
at#an#age#of#only#2#Myr.#Two#of#the#new#planets#are#similarly#located#to#those#inferred#in#the#
famous#HL#Tau#protoplanetary#disc;#in#CI#Tau,#additional#observational#data#enables#a#more#
complete#analysis#of#the#system#properties#than#was#possible#for#HL#Tau.#Our#dust#and#gas#
dynamical#modeling#satisfies#every#available#observational#constraint#and#points#to#the#most#
massive#ensemble#of#exoJplanets#ever#detected#at#this#age,#with#its#four#planets#spanning#a#
factor#1000#in#orbital#radius.Our#results#show#that#the#association#between#hot#Jupiters#and#gas#giants#on#wider#orbits,#observed#in#older#stars,#is#apparently#in#place#at#an#early#
evolutionary#stage.#

#12

MagneCcally$induced$terminaCon$of$giant$planet$formaCon$$

Here$a$physical$model$for$terminating$giant$planet$formation$is$outlined$and$compared$to$other$methods$of$late5stage$giant$planet$formation.$As$has$been$pointed$out$before,$gas$
accreting$into$a$gap$and$onto$the$planet$will$encounter$the$planetary$dynamo5generated$magnetic$field.$The$planetary$magnetic$field$produces$an$effective$cross$section$through$which$gas$is$accreted.$Gas$outside$this$cross$section$is$recycled$into$the$protoplanetary$disk,$hence$only$a$fraction$of$mass$that$is$accreted$into$the$gap$remains$bound$to$the$planet.$This$cross$section$inversely$scales$with$the$planetary$mass,$which$naturally$leads$to$stalled$planetary$growth$late$in$the$formation$process.$We$show$that$this$method$naturally$leads$to$
Jupiter5mass$planets$and$does$not$invoke$any$artificial$truncation$of$gas$accretion,$as$has$
been$done$in$some$previous$population$synthesis$models.$The$mass$accretion$rate$depends$
on$the$radius$of$the$growing$planet$after$the$gap$has$opened,$and$we$show$that$so5called$
hot5start$planets$tend$to$become$more$massive$than$cold5start$planets.$When$this$result$is$combined$with$population$synthesis$models,$it$might$show$observable$signatures$of$cold5
start$versus$hot5start$planets$in$the$exoplanet$population.$

#13

Simultaneous#spectral#energy#distribu`on#and#nearEinfrared#
interferometry#modeling#of#HD#142666#

We#present#comprehensive#models#of#Herbig#Ae#star,#HD#142666,#which#aim#to#
simultaneously#explain#its#spectral#energy#distribution#(SED)#and#nearEinfrared#(NIR)#
interferometry.#Our#new#submilliarcsecond#resolution#CHARA#(CLASSIC#and#CLIMB)#
interferometric#observations,#supplemented#with#archival#shorter#baseline#data#from#
VLTI/PIONIER#and#the#Keck#Interferometer,#are#modeled#using#centroEsymmetric#geometric#models#and#an#axisymmetric#radiative#transfer#code.#CHARAs#330#m#baselines#enable#us#to#
place#strong#constraints#on#the#viewing#geometry,#revealing#a#
disk#inclined#at#58 from#faceEon#with#a#160 major#axis#position#angle.#Disk#models#imposing#vertical#hydrostatic#equilibrium#provide#poor#fits#to#the#SED.#Models#accounting#for#disk#scale#height#inflation,#possibly#induced#by#turE bulence#associated#with#magnetoErotational#
instabilities,#and#invoking#grain#growth#to#>∼1#μm#size#in#the#disk#rim#are#required#to#
simultaneously#reproduce#the#SED#and#measured#visibility#profile.#However,#visibility#
residuals#for#our#best#model#fits#to#the#SED#indicate#the#presence#of#unexplained#NIR#
emission,#particularly#along#the#apparent#disk#minor#axis,#while#closure#phase#residuals#
indicate#a#more#centroEsymmetric#emitting#region.#In#addition,#our#inferred#58 disk#inclination#is#inconsistent#with#a#diskEbased#origin#for#the#UX#OriEtype#variability#exhibited#by#
HD#142666.#Additional#complexity,#unaccounted#for#in#our#models,#is#clearly#present#in#the#
NIREemitting#region.#We#propose#the#disk#is#likely#inclined#toward#a#more#edgeEon#orientation#
and/or#an#optically#thick#outflow#component#also#contributes#to#the#NIR#circumstellar#flux.#

#15 Multiple$Disk$Gaps$and$Rings$Generated$by$a$Single$SuperAEarth:$
II.$Spacings,$Depths,$and$Number$of$Gaps,$with$Application$to$
Real$Systems$
ALMA$has$found$multiple$dust$gaps$and$rings$in$a$number$of$protoplanetary$disks,$including$
HL$Tau$and$TW$Hya,$in$continuum$emission$at$millimeter$wavelengths.$The$origin$of$such$
structures$is$in$debate.$Recently,$we$documented$how$one$superAEarth$planet$can$open$
multiple$(up$to$five)$dust$gaps$in$a$disk$with$low$viscosity$(α$<∼ 10−4).$In$this$paper,$we$
examine$how$the$positions,$depths,$and$total$number$of$gaps$opened$by$one$planet$depend$
on$input$parameters,$and$apply$our$results$to$real$systems.$Gap$locations$(equivalently,$spacings)$are$the$easiest$metric$to$use$when$making$comparisons$between$theory$and$observations,$as$positions$can$be$robustly$measured.$We$fit$the$locations$of$gaps$empirically$
as$functions$of$planet$mass$and$disk$aspect$ratio.$We$find$that$the$locations$of$the$double$
gaps$in$HL$Tau$and$TW$Hya,$and$of$all$three$gaps$in$HD$163296,$are$consistent$with$being$
opened$by$a$subASaturn$mass$planet.$This$scenario$predicts$the$locations$of$other$gaps$in$HL$
Tau$and$TW$Hya,$only$some$of$which$appear$consistent$with$current$observations.$We$also$
show$how$the$Rossby$wave$instability$may$develop$at$the$edges$of$several$gaps$and$result$in$
multiple$dusty$vortices,$all$caused$by$one$planet.$A$planet$as$low$in$mass$as$Mars$may$
produce$multiple$dust$gaps$in$the$terrestrial$planet$forming$region.$#17 The(Gaia(DR2(view(of(the(Gamma(Velorum(cluster:(resolving(the(6D(structureGaia$ESO(Survey(observa1ons(of(the(young(Gamma(Velorum(cluster(led(to(the(discovery(of(two(kinema1cally(dis$1nct(popula1ons,(Gamma(Vel(A(and(B,(respec1vely,(with(popula1on(B(extended(over(several(square(degrees(in(theVela(OB2(associa1on.(Using(the(Gaia(DR2(data(for(a(sample(of(high$probability(cluster(members,(we(ﬁnd(that(thetwo(popula1ons(diﬀer(not(only(kinema1cally,(but(are(also(located(at(diﬀerent(distances(along(the(line(of(sight,(withthe(main(cluster(Gamma(Vel(A(being(closer.(A(combined(ﬁt(of(the(two(popula1ons(yields(̟A(=(2.895( 0.008(mas(and(̟B(=(2.608( 0.017(mas,(with(intrinsic(dispersions(of(0.038( 0.011(mas(and(0.091( 0.016(mas,(respec1vely.(Thistranslates(into(distances(of(345.4+1.0+12.4(pc(and(383.4+2.5+15.3(pc,(respec1vely,(showing(that(Gamma(Vel(A(is(closer(−1.0−11.5(−2.5−14.2(than(Gamma(Vel(B(by(∼ 38(pc.(We(ﬁnd(that(the(two(clusters(are(nearly(coeval,(and(that(Gamma(Vel(B(is(expanding.(We(suggest(that(Gamma(Vel(A(and(B(are(two(independent(clusters(located(along(the(same(line(of(sight.

#18Synthetic)[CII])emission)maps)of)a)simulated)molecular)cloud)in)formation)

The C+ ion is an important coolant of interstellar gas, and so the [CII] fine structure line isfrequently observed in the interstellar medium. However, the physical and chemical properties of the[CII]-emitting gas are still unclear. We carry out non-LTE radiative transfer simulations with RADMC3D to study the [CII] line emission from a young, turbulent molecular cloud before the onset of starformation, using data from the SILCC-Zoom project. The [CII] emission is optically thick over 40% ofthe observable area with I[CII]>0.5 K km s−1. To determine the physical properties of the [CII]
emitting gas, we treat the [CII] emission as optically thin. We find that the [CII] emission originates
primarily from cold, moderate density gas (40≲T≲65 K and 50≲n≲440 cm−3), composed mainly ofatomic hydrogen and with an effective visual extinction between ∼0.50 and ∼0.91. Gas dominated bymolecular hydrogen contributes only ≲20% of the total [CII] line emission. Thus, [CII] is not a goodtracer for CO-dark H2 at this early phase in the cloud's lifetime. We also find that the total gas, Hand C+ column densities are all correlated with the integrated [CII] line emission, with power law
slopes ranging from 0.5 to 0.7. Further, the median ratio between the total column density and the[CII] line emission is YCII≈1.11021 cm−2 (K km s−1)−1, and YCII scales with I−0.3[CII]. We
expect YCII to change in environments with a lower or higher radiation field than simulated here.