Imaging he dis ibu ion o wa e apou
in plane - o ming disks wi h ALMA
S e ano Facchini
Uni e si y o Milan
UNVEIL
101076613
Dis ibu ion o wa e apou in p o oplane a y disks
S a ic disk model, passi ely hea ed by a cen al He big s a :
de ines a clea snow su ace (snowline in he disk midplane)
No su+2017
A “blu ed” snow su ace
When including mo e physics beyond a s a ic model,
he ansi ion be ween gas and ice ese oi s becomes mo e blu ed
Banza i+in p ep., ARA&A e iew
Image c edi : Banza i+, Go don con e ence
Di e en ese oi s o wa e gas in a disk
gas
H
α
Rese oi 1:
he mally deso bed
wa e
gas
H
α
gas
H
α
Rese oi 2:
pho odeso bed
wa e
Rese oi 3:
e o med wa e
Image c edi : M. Leemke
wa e
snowline
~ 1-10 au
Th ee di e en ese oi s o wa e apou
depending on T and UV pene a ion dep h
A he mal g adien in he snow su ace
Kamp+2021, Banza i+2023a,b
Dis inc wa eleng h egimes ypically sensi i e o di e en uppe ene gy le els,
acing di e en adial anges
Why do we ca e?
Wa e snowline can p omo e plane esimal o ma ion.
High H2O abundance in inne egions may be due o high pebble lux, a key
pa ame e egula ing pebble acc e ion in he o ma ion o plane a y co es and
ocky plane s.
Loca ion o wa e snowline leads o d as ic changes in elemen al a ios (e.g., C/O)
o ice and solid phases.
Wa e iso opologue a io is a key ace o ice ep ocessing du ing he disk
o ma ion phase.
Why do we ca e?
Wa e snowline can p omo e plane esimal o ma ion
High H2O abundance in inne egions may be due o high pebble lux, a key
pa ame e egula ing pebble acc e ion in he o ma ion o plane a y co es and
ocky plane s
Loca ion o wa e snowline leads o d as ic changes in elemen al a ios (e.g., C/O)
o ice and solid phases
Wa e iso opologue a io is a key ace o ice ep ocessing du ing he disk
o ma ion phase.
Complemen a y app oaches o cons ain wa e apou ex en
Banza i+2023, B i an+2016, Leemke +in p ep.
JWST: mul iple ansi ions in NIR-MIR,
he mally “ esol e” g adien s om exci a ion
s udies
i-Shell, CRIRES+: High- es NIR spec oscopy,
spec ally esol e indi idual lines, econs uc
in ensi y p o ile wi h Dopple omog aphy
ALMA: high angula esolu ion in (sub-)mm
egime, spec ally and spa ially esol e
indi idual lines, and access o iso opologues
Complemen a y app oaches o cons ain wa e apou ex en
Banza i+2023, B i an+2016, Leemke +in p ep.
JWST: mul iple ansi ions in NIR-MIR,
he mally “ esol e” g adien s om exci a ion
s udies
i-Shell, CRIRES+: High- es NIR spec oscopy,
spec ally esol e indi idual lines, econs uc
in ensi y p o ile wi h Dopple omog aphy
ALMA: high angula esolu ion in (sub-)mm
egime, spec ally and spa ially esol e
indi idual lines, and access o iso opologues
De ec ion o wa e main iso opologue wi h ALMA in HL Tau
Eup ~ 205 K
Eup ~ 470 K
Eup ~ 1860 K 60 mas esolu ion
Facchini+2024, Na . As .
, 183 GHz
, 325 GHz
, 321 GHz
500 mas esolu ion
500 mas esolu ion
Conclusions
•Disks a e la gely subs uc u ed in hei kinema ical pa e n, spi als being mo e
common han in mm con inuum and sca e ed ligh emission
•Signa u es o Jupi e mass plane -disk in e ac ions in ou e egions
•E idence o disk dynamics ye o be iden i ied
•New me hodology o es ima ing disk masses wi h new o hogonal app oaches
•Plane -induced s uc u e can a ec he chemis y o he hos ing disk
•Main H2O iso opologue can be used o map wa e apou in b igh disks
C edi : ALMA (ESO/NAOJ/NRAO)/S. Facchini e al.
New 50mas da a o he 183 GHz line
Leemke +subm.
We de ec wa e ou o la ge
adii (snowline a ~5 au),
abo e he wa e snow-su ace
Lines look close o he mal,
bu ha d o ully cons ain.
The ole o con inuum op ical dep h
Leemke +subm.
The ole o con inuum op ical dep h
Leemke +subm.
The ole o con inuum op ical dep h
Leemke +subm.
Exci a ion seems easonably close o LTE when accoun ing o con inuum op ical
dep h. Lines in he FIR a e sensi i e o <1% o he wa e , in he mm o ~50%.
A di ec ly-i adia ed ca i y wall
Rampinelli+subm.
Spa ially esol ed H216O de ec ed in he ca i y o he HD 100546 disk.
A di ec ly-i adia ed ca i y wall
Leemke +2021, Rampinelli+subm.
The p o ile o he wa e emission peaks jus inside he dus ca i y wall:
RT models indica e dus empe a u es abo e H2O sublima ion empe a u e
Wha is he scalabili y o hese obse a ions?
This s udy can be pe o med only on b igh es disks
(~10 no ou bu s ing, ~20 ou bu s ing),
he limi is line sensi i i y.
Simplis ic a gumen s yield:
(scaling is s eep wi h …)
FH2O∼L1/2
*
M*
We need a massi e boos in line sensi i i y/collec ing a ea,
a nex -gene a ion ALMA:
CAD model o ng-VLA an enna,
cou esy o m ex indus y;
SKA-mid an enna design
Conclusions
1) Wa e iso opologues (H2O, H218O, HDO, D2O) can be de ec ed in b igh
plane - o ming disks
2) The mally deso bed gas indica es inhe i ance scena io (D2O/H2O)
3) (Sub-)mm lines a e op imal o p obe he bulk o wa e column densi y and ge
close o he midplane wa e snowline
4) T ansi ion disks (wi h wa m ca i y walls) a e op imal a ge s o cons ain H2O/
COM a ios in he mally deso bed gas.
5) A adically upg aded mm in e e ome e needed in he u u e o ex end he
s udy o la ge samples.
