Fu u e pe spec i es wi h cm obse a ions:
SKA and ngVLA
Izaskun Jimenez-Se a (CSIC)
Cen e o As obiology (Spain)
Towa ds new F on ie s: he As ochemical Jou ney om Young S ella Nu se ies o Exoplane s - ESO – 13 Ma 2025
Ou line:
•Why cm wa eleng hs?
•Specs o he SKA and ngVLA
•Key science wi h he SKA and ngVLA
Ou line:
•Why cm wa eleng hs?
•Specs o he SKA and ngVLA
•New science wi h he SKA and ngVLA
(1) Dus emission is op ically hin and less a ec ed by sca e ing
Why cm wa eleng hs?
Ca asco-González+2019
HL Tau
(1) Dus emission is op ically hin and less a ec ed by sca e ing
Why cm wa eleng hs?
HL Tau
See also Zhu+2019
Ca asco-González+2019
(1) Dus emission is op ically hin and less a ec ed by sca e ing
Why cm wa eleng hs?
HL Tau
See also Zhu+2019
Ca asco-González+2019
(1) Dus emission is op ically hin and less a ec ed by sca e ing
Why cm wa eleng hs?
Zhu+2019
A la ge ac ion o he disk mass emains hidden a mm 𝛌’s
(2) Molecula line emission una ec ed by dus op ical dep h
Why cm wa eleng hs?
de Simone+2017
NGC1333 IRAS4A IRAM PdB @1.4mm
CH3OH wi h VLA @25 GHz
Molecula
emission
sc eened by
la ge dus opaci y
a mm 𝛌’s
Ou line:
•Why cm wa eleng hs?
•Specs o he SKA and ngVLA
•New science wi h he SKA and ngVLA
Figu es o me i o SKA-MID:
AA4 𝛔c=2.4 𝜇Jy/beam, @12 GHz in 1h wi h 𝛥𝜈=3.6 GHz, 𝜃beam=34 mas
𝛔L=560 𝜇Jy/beam, @12 GHz in 1h wi h 𝛥 =10km/s, 𝜃beam=34 mas
Figu es o me i o ngVLA:
𝛔c=0.24 𝜇Jy/beam, @16 GHz in 1h wi h 𝛥𝜈=3.6 GHz, 𝜃beam=0.43 mas
𝛔L=20 𝜇Jy/beam, @16 GHz in 1h wi h 𝛥 =10km/s, 𝜃beam=0.43 mas
Ou line:
•Why cm wa eleng hs?
•Specs o he SKA and ngVLA
•New science wi h he SKA and ngVLA
Key science a cm wa eleng hs
1) How do ocky plane s o m? 2) How did li e o igina e?
3) Wha a e exoplane s like?
Key science a cm wa eleng hs
1) How do ocky plane s o m?
How Do Rocky Plane s Fo m?
Tychoniec+2020
Galame z+2019
Challenge:
How do we p obe g ain
g ow h beyond he dus
cen ime e -size ba ie ?
•Fo ma ion o ocky co es o plane s ia g ain g ow h and dus se ling
How Do Rocky Plane s Fo m?
Tes i e al. 2014 Hoa e e al. 2015
SKA and ngVLA co e he igh λ’s o p obe cm-sized g ains
Cha ac e izing he mul iple p o os ella sys em VLA 1623-2417
Radley+2025
Class 0 YSOs
(e.g.
Mu illo+2013,2018
Sada oy+2019,2024)
Class I YSOs
(Me cimek+2023
Michel+2022
Sada oy+2019,2024)
Radley+2025
Some o he highes angula
esolu ion images ob ained
wi h he VLA
Q, K and X-bands
A con igu a ion
𝜃beam=0.06”-0.4”
Radley+2025
Some o he highes angula
esolu ion images ob ained
wi h he VLA
Q, K and X-bands
A con igu a ion
𝜃beam=0.06”-0.4”
G ain g ow h wi h
amax>1mm
amax uncons ained due
o he poo VLA’s 𝜃beam
a low 𝜈’s
signi ican con ibu ion
o ionized gas
a 𝜈<15 GHz
P imo dial RNA-wo ld chemical scheme (Powne +2009; Pa el+2015)
Towa d he RNA-wo ld in he ISM
RNA
P ecu so s
Suga s
&
Lipid
p ecu so s
Amino Acids
Py imidine
ibonucleo ides
(building blocks
o RNA)
Towa d he RNA wo ld in he ISM
(Jiménez-Se a+2020, As obiology, 20,1048J)
Py imidine
ibonucleo ides
Towa d he RNA wo ld in he ISM
Py imidine
ibonucleo ides
Zeng e al.
(2019)
(Jiménez-Se a+2020, As obiology, 20,1048J)
G0693-0.027
G+0.693-0.027
Quiescen cloud (no signs o s a - o ma ion) unde going
a cloud-cloud collision
(Hasegawa+94;Sa o+00; Tsuboi+15; Wu+17; Zeng+20; A mijos-Abendaño+20)
❑n(H2)~4x104 cm-3
❑Tdus <20 K s. Tgas>100 K
❑Low Tex o he molecula gas (<15 K).
❑Huge ad an age o COM sea ches in “c owded” spec al su eys
G+0.693 s. Sg B2 (N2)
Jimenez-Se a, Codella, Belloche 2025
(Chap e on “Obse a ions o COMs” o Handbook o As ochemis y)
G+0.693 is iche in unsa u a ed and S-bea ing species
High CRIR enhances ion and a omic abundance
(see San ama ía e al. 2021; Ri illa+2022; Sanz-No o+2024; Rey-Mon ejo+ in p ep.)
he Onse o P ebio ic chEmis y iN Space
38
A) Wha p ebio ic
molecules o m in
he ISM?
B) Wha molecules a e inhe i ed
om he pa en al molecula co e?
C) Wha is he o igin o he
chemical complexi y in he ISM?
PI: I. Jiménez-Se a
Wha can he SKA and ngVLA do o us?
SKA and ngVLA as de ec o s o p ebio ic COMs:
1) cm ’s a e “cleane ” (less line con usion and line blending)
2) in e e ome y “na u ally” educes linewid hs
Ex ended COM- ich GMC
(G+0.693)
B igh HII egion (L sou ce)
Jimenez-Se a e al. (2022)
See also Schoedel e al. (2024) – SKA Galac ic Cen e Su ey
Feasibili y s udy o C3 and C4 suga s wi h SKA
P ebio ic Molecules wi h SKA
Glyce aldehyde
de ec ed wi hin a
ew ens o hou s
wi h SKA Band 5a/5b
in i s AA*
con igu a ion
SKA and ngVLA p o ide a b igh u u e!!
Wo ds o cau ion:
•Con inuum emission: combina ion o dus he mal, ee- ee and
synch o on con ibu ions -> hey need o be disen angled (RRLs,
ool o es ima ing ee- ee emission om ionized gas)
•Expec high a iabili y (Cou ens e al. 2019) -> mul i-epoch
obse a ions a e a mus
•Fo line emission, non-LTE e ec s may be p esen (Fau e e al.
2014,2018) -> his shows he need o molecula collisional
coe icien s (especially o COMs)
AEI
(PID2022-136814NB-I00)
ILINK CSIC
(p ojec # 23017)
THANK YOU!!
