Chemical Signa u es o a p es ella clus e
in he Galac ic Cen e
Lau a Colzi
(Cen o de As obiología, CSIC-INTA)
Ma ch 10 h 2025
J. Ma ín-Pin ado, S. Zeng, I. Jiménez-Se a,V. M. Ri illa, Sanz-No o, M. and many o he s...
G an PID2022-136814NB-I00 unded by:
He schel PACS 70 µm image o he Galac ic cen e egion. Molina i e al. (2001)
The CMZ con ains 80% o he
dense molecula gas in he
Galaxy
BUT
he ecen s a o ma ion a e is one o de
o magni ude lowe han ha in he disk
(e.g. Longmo e e al. 2013; Ba nes e al. 2017)
ØHigh le el o u bulence due o he la ge in e nal cloud eloci y
dispe sion (∼15–50 km s−1)
AND
ØWidesp ead high kine ic empe a u es (Tkin om ∼50 K o >100 K)
EXTREME ENVIRONMENTAL CONDITIONS
could p e en s a o ma ion
Image C edi : adio image om Mee KAT. Ian Heywood (Ox o d U.), SARAO; Colo P ocessing: Juan Ca los Munoz-Ma eos (ESO)
ØHigh le el o u bulence due o he la ge in e nal cloud eloci y
dispe sion (∼15–50 km s−1)
AND
ØWidesp ead high kine ic empe a u es (Tkin om ∼50 K o >100 K)
EXTREME ENVIRONMENTAL CONDITIONS
could p e en s a o ma ion
BUT do no s op i en i ely
à Sg B2 and Sg C, A ches, Quin uple , he B ick (e.g. Longmo e+2013b;
Walke +2021)
Image C edi : adio image om Mee KAT. Ian Heywood (Ox o d U.), SARAO; Colo P ocessing: Juan Ca los Munoz-Ma eos (ESO)
Image C edi : adio image om Mee KAT. Ian Heywood (Ox o d U.), SARAO; Colo P ocessing: Juan Ca los Munoz-Ma eos (ESO)
ØLa ge column densi ies o wa m and u bulen gas
Mo eo e …
àDi icul o disen angle signa u es o dense and less
u bulen p es ella co es
Image C edi : adio image om Mee KAT. Ian Heywood (Ox o d U.), SARAO; Colo P ocessing: Juan Ca los Munoz-Ma eos (ESO)
ØLa ge column densi ies o wa m and u bulen gas
Mo eo e …
àDi icul o disen angle signa u es o dense and less
u bulen p es ella co es
HOW o iden i y and s udy he ea lie e olu iona y s ages o he
dense, cold, and quiescen p es ella co es, i p esen ?
He schel PACS 70 µm image o he Galac ic cen e egion. Molina i e al. (2001)
Lau a Colzi
A CMZ SOURCE: G+0.693-0.027
Lau a Colzi
A CMZ SOURCE: G+0.693-0.027
A naud Belloche’s
alk
omo ow
Lau a Colzi
A CMZ SOURCE: G+0.693-0.027
Colzi e al. (2022a), ApJL, 926, L22Lau a Colzi
Objec i e à D/H a ios o
HCN, HNC, HCO+ and
N2H+
App oach à Use o mul iple
o a ional ansi ions
Colzi e al. (2022a), ApJL, 926, L22Lau a Colzi
Objec i e à D/H a ios o
HCN, HNC, HCO+ and
N2H+
App oach à Use o mul iple
o a ional ansi ions
Disco e à 2 line
componen s needed
Colzi e al. (2022a), ApJL, 926, L22
P esence o wo di e en line
componen s:
1. Tu bulen (FWHM = 20 km s-1)
componen (Tex=7 K)
Typical o he CMZ
2. Less u bulen (FWHM = 9 km s-1)
componen (Tex=3-4 K)
à Ve y clea om high-J ansi ions
Lau a Colzi
V ad (km s-1)V ad (km s-1)
Ta* (K)
Ta* (K)
BROAD COMPONENT
NARROW COMPONENT COSMIC D/H = 2.55 x 10-5
1. D/H[HCN, HNC] > cosmic D/H
D/H[HCO+, N2H+] à cosmic D/H
2. D/H[HCN, HNC, HCO+, N2H+] >
cosmic D/H
Colzi e al. (2022), ApJL, 926, L22Lau a Colzi
DEUTERIUM FRACTIONATION
Lau a Colzi
Low- empe a u e Iso opic-exchange eac ions
GAS-PHASE
Colzi e al. (2022), ApJL, 926, L22
H3++ HDH2D++ H2+ 232 K
CH3++ H
D
CH2
D
++ H2+654 K
C2H2++ H
D
C2H
D
++ H2+ 550 K
Ø o T≤30 K: D/H o N2H+, HCN, HNC, HCO+ enhanced
Ø o T>70-80 K: D/H o HCN and HNC enhanced
(Roue +2007, Roue +2013)
o ypical n o CMZ
(~103-105cm-3, e.g.
Ginsbu g+2016)
e.g. He bs (2003),
Roue e al. (2013)
DEUTERIUM FRACTIONATION
T ≤30 K à
T > 70 K à
BROAD COMPONENT
NARROW COMPONENT COSMIC D/H = 2.55 x 10-5
1. D/H[HCN, HNC] > cosmic D/H
D/H[HCO+, N2H+] à cosmic D/H
Consis en wi h T>70 K
2. D/H[HCN, HNC, HCO+, N2H+] >
cosmic D/H
Colzi e al. (2022), ApJL, 926, L22Lau a Colzi
Tempe a u e ≤30 K o he
na ow componen
DEUTERIUM FRACTIONATION
Colzi e al. (2022a), ApJL, 926, L22
P esence o wo di e en line
componen s:
1. Tu bulen (FWHM = 20 km s-1),
wa m (Tkin~100 K) and less dense
(n
⋆
~0.3-3x104 cm-3) componen
Gas componen ypical o he CMZ
⋆" om non-LTE analysis (RADEX,
an de Tak+2007)
Lau a Colzi
V ad (km s-1)V ad (km s-1)
Ta* (K)
Ta* (K)
NON-LTE analysis
Colzi e al. (2022a), ApJL, 926, L22
P esence o wo di e en line
componen s:
1. Tu bulen (FWHM = 20 km s-1),
wa m (Tkin~100 K) and less dense
(n
⋆
~0.3-3x104 cm-3) componen
Gas componen ypical o he CMZ
2. Less u bulen (FWHM = 9 km s-1),
colde (Tkin~20-30 K) and dense
componen (n
⋆"
~0.05-1x106 cm-3)
Dense and colde gas componen
à On he e ge o s a o ma ion?
⋆" om non-LTE analysis (RADEX,
an de Tak+2007)
Lau a Colzi
V ad (km s-1)V ad (km s-1)
Ta* (K)
Ta* (K)
NON-LTE analysis
Lau a Colzi
Exci a ion and spa ial s udy owa ds G+0.693
Lau a Colzi
Exci a ion and spa ial s udy owa ds G+0.693
70-85 km s-1
Single pixels (0.18 pc) FWHM 1.3 –4.9 km s-1
Colzi e al. (2024), A&A, 690, A121
Lau a Colzi
Exci a ion and spa ial s udy owa ds G+0.693
C2 will no agmen and possibly expand
C3 can ei he collapse o u he agmen
70-85 km s-1
Single pixels (0.18 pc) FWHM 1.3 –4.9 km s-1
Colzi e al. (2024), A&A, 690, A121
CONCLUSIONS
BROAD COMPONENT
NARROW COMPONENT COSMIC D/H = 2.55 x 10-5
Ou da a sugges ed he p esence o a p es ella condensa ion in he
Cen al Molecula Zone (CMZ) ha migh be on he e ge o he collapse
Colzi e al. (2022a,2024)
Lau a Colzi
C3
80-85 km s-1
70-75 s 80-85 km s-1
C3
C2 C2
Chemical Signa u es o a p es ella clus e
in he Galac ic Cen e
Lau a Colzi
(Cen o de As obiología, CSIC-INTA)
Ma ch 10 h 2025
J. Ma ín-Pin ado, S. Zeng, I. Jiménez-Se a,V. M. Ri illa, Sanz-No o, M. and many o he s...
G an PID2022-136814NB-I00 unded by:
BACK UP SLIDES
ACES ALMA LARGE PROGRAM
Inne 100 pc o he CMZ co e ed a 1.5’’ (0.05 pc) o esolu ion in Band 3
To al ime alloca ion: 112 h s (12m) + 7m and TP
om he la ges scales (12m+7m+TP) o indi idual co es (~1.5’’à0.05 pc)
Lau a Colzi
Main PI: S e en Longmo e
WP3: Chemis y and Physical Modeling
Goals
De e mina ion o he physical and chemical p ope ies o he dus , molecula gas and
ionized gas s uc u es mapped wi h ACES
om he la ges scales (12m+7m+TP) o indi idual co es (~1.5’’à0.06 pc)
Lau a Colzi and Izaskun Jiménez-Se a
(Cen o de As obiología, CSIC-INTA)
Con ac us @: [email protected] a-csic.es [email p o ec ed]-csic.es
Spec al Se up and Molecules Co e ed
C edi s: Elisabe h Mills
Lau a Colzi
Dense gas ace s
(HCO+, HCN, CS)
Shock ace s
(SiO, HNCO, SO)
PDR ace s
(HCO)
Ionized gas
(H40a)
Ho co es
(HC3N*, COMs)
6 spec al windows:
A i s example: mm1 and mm2 (ho )co es in Sg C
Lau a Colzi
Molecules iden i ied so a owa ds mm1:
HC15N, HN13C, H13CN,HC3N (cyanoace ylene), HC13CCN, HCC13CN, H13CO+,HCO+,
HN13CO, HNCO (isocyanic acid), CS, SO, 34SO,SiO,HC5N (cyanodiace ylene),
C2H5CN (p op ioni ile), H2CCO (ke ene), CCS, NH2CN (cyanamide),
CH3OCHO (me hyl o ma e), C2H5OH (e hanol), CH3OCH3(dime hyl e he ),
CH3SH (me hane hiol o me hyl me cap an), CH3NCO (me hyl isocyana e), CH3CHO
(ace aldehyde), H2CO ( o maldehyde), CH3OH (me hanol),
HC3N 6=1, 7=1, HC3N 7=2, HC(O)NH2( o mamide), CH318OH
70-80 km s-1
40-50 km s-1 50-60 km s-1
60-70 km s-1
Hole
Massi e cloud
Shell
Massi e cloud
Lau a Colzi
Exci a ion and spa ial s udy owa ds G+0.693
HNCO(40,4-30,3)
IRAM 30m MAPS
10 pc
See also
Hasegawa+1994;
Sa o+2000;
Zeng+2020;
A mijos-Abendaño+2020;
Enokiya & Fukui 2022
Colzi e al. (2024), A&A, 690, A121
Beyond ou Galaxy…
Lau a Colzi
Galaxy NGC 253
Bu e wo h, J., .., Colzi, L., e al.: A&A, 693, A65 (2025)
