A ilia ions:
1 2
lenna -boehm.de
[email p o ec ed]
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM
SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND
OUTFLOWS?
CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc
10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0
2
4
6
8
10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10
0
50
10
20
30
40
υLSR [km s−1]
–10
0
50
10
20
30
40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]
υLSR [km s−1]
–70
–60
–10
–50
–40
–30
–20
–70
–60
–10
–50
–40
–30
–20
IRAS 12326–6245
ou low
SO
+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s
39s
36s
33s
30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR
+
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM
SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0
2
4
6
8
10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]υLSR [km s−1]
70 80 13090 100 110 12070 80 13090 100 110 120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10 05010 20 30 40
υLSR [km s−1]
–10 05010 20 30 40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]υLSR [km s−1]
–70 –60 –10–50 –40 –30 –20 –70 –60 –10–50 –40 –30 –20
IRAS 12326–6245
ou low
SO+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM
SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0
2
4
6
8
10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]υLSR [km s−1]
70 80 13090 100 110 12070 80 13090 100 110 120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10 05010 20 30 40
υLSR [km s−1]
–10 05010 20 30 40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]υLSR [km s−1]
–70 –60 –10–50 –40 –30 –20 –70 –60 –10–50 –40 –30 –20
IRAS 12326–6245
ou low
SO+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM
SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc
10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0
2
4
6
8
10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]υLSR [km s−1]
70 80 13090 100 110 12070 80 13090 100 110 120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10 05010 20 30 40
υLSR [km s−1]
–10 05010 20 30 40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]υLSR [km s−1]
–70 –60 –10–50 –40 –30 –20 –70 –60 –10–50 –40 –30 –20
IRAS 12326–6245
ou low
SO+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0 2 4 6 8 10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10
0
50
10
20
30
40
υLSR [km s−1]
–10
0
50
10
20
30
40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]
υLSR [km s−1]
–70
–60
–10
–50
–40
–30
–20
–70
–60
–10
–50
–40
–30
–20
IRAS 12326–6245
ou low
SO
+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR
+
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0 2 4 6 8 10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10
0
50
10
20
30
40
υLSR [km s−1]
–10
0
50
10
20
30
40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]
υLSR [km s−1]
–70
–60
–10
–50
–40
–30
–20
–70
–60
–10
–50
–40
–30
–20
IRAS 12326–6245
ou low
SO
+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR
+
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND OUTFLOWS? CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0 2 4 6 8 10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10
0
50
10
20
30
40
υLSR [km s−1]
–10
0
50
10
20
30
40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]
υLSR [km s−1]
–70
–60
–10
–50
–40
–30
–20
–70
–60
–10
–50
–40
–30
–20
IRAS 12326–6245
ou low
SO
+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s39s36s33s30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
Kobayashi, C., Ka akas, A. I., & Umeda, H. (2011). The e olu ion o iso ope a ios in he Milky Way Galaxy. MNRAS, 414(4), 3231-3250.
Maas, Z. G., & Pilachowski, C. A. (2021). The Galac ic Chemical E olu ion o Chlo ine. AJ, 161(4), 183.
Mölle , T., End es, C., & Schilke, P. (2017). eX ended CASA line analysis so wa e sui e (XCLASS). A&A, 598, A7.
Neu eld, D. A., & Wol i e, M. G. (2009). The chemis y o in e s ella molecules con aining he halogen elemen s. ApJ, 706(2), 1594.
Neu eld, D. A. e al. (2021). The Chemis y o Chlo ine-Bea ing Species in he Di use In e s ella Medium, and New SOFIA/GREAT*
Obse a ions o HCl+. ApJ, 917(2), 104.
Reid, M. J. e al. (2019). T igonome ic pa allaxes o high-mass s a - o ming egions: ou iew o he Milky Way. ApJ, 885(2), 131.
Re e ences:
CHLORINE: PROBING THE ISM SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND
OUTFLOWS?
CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0 2 4 6 8 10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10 05010 20 30 40
υLSR [km s−1]
–10 05010 20 30 40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]υLSR [km s−1]
–70 –60 –10–50 –40 –30 –20 –70 –60 –10–50 –40 –30 –20
IRAS 12326–6245
ou low
SO+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s
39s
36s
33s
30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
A ilia ions:
1 2
lenna -boehm.de
lenna [email protected] g
✉
T acing Chlo ine Iso opes Ac oss he Milky Way
A La ge Scale Su ey o Hyd ogen Chlo ide in S a -Fo ming Regions
A shia M. Jacob2, F ied ich Wy owski2, Ka l M. Men en2, Ashley T. Ba nes1, Ka ha ina Imme 1
HCl IN ALL TARGETS!
Lenna Böhm1,2
Lenna Böhm, ESO
IMPRS PhD s uden
SCAN ME!
Böhm, L. e al., in p ep., T acing chlo ine iso opes ac oss he Milky Way
Elia, D. e al. (2021). The Hi-GAL compac sou ce ca alogue–II. The 360° ca alogue o clump physical p ope ies. MNRAS, 504(2),
2742-2766.
Gianne i, A. e al.(2014). ATLASGAL-selec ed massi e clumps in he inne Galaxy-I. CO deple ion and iso opic a ios. A&A, 570, A65.
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Re e ences:
CHLORINE: PROBING THE ISM SURVEYING HCl
WHAT WE STILL DON'T KNOW
SCATTERED, NO TREND
OUTFLOWS?
CONTACT
Image c edi : apex- elescope.o g
H2
H2
e
hω
Cl+
HCl+
Cl
H2Cl+
HCl
hω
e
e
e
Chlo ine iso opes p obe he nucleosyn hesis
his o y o massi e s a - o ming egions and
hei en ichmen o he ISM:
‣35Cl and 37Cl a e p oduced in co e-collapse
supe no ae (CCSNe) and he weak s-p ocess
in massi e s a s (Maas & Pilachowski, 2021)
‣The 35Cl/37Cl a io in a CCSN a ies wi h
ac o s such as ini ial mass, me allici y, and
explosion p ope ies (Maas & Pilachowski, 2021)
‣Galac ic chemical e olu ion models p edic he
iso opic a io o a y wi h me allici y, hence
acing he nucleosyn hesis his o y o a
galaxy (Kobayashi e al. 2010)
28 massi e s a - o ming egions
ac oss he Milky Way
‣b igh sub-mm con inuum sou ces
(Hi-Gal ca alogue; Elia e al., 2021)
‣Galac ocen ic adii be ween
o (Reid e al., 2019)
‣selec ed om he HyGAL and
PRISMAS su eys on hyd ides
0.1 kpc 10 kpc
and he SEPIA660 ecei e
•single-pixel, sideband sepa a ed he e odyne
•na i e esolu ion:
‣smoo hed o
0.03 km s−1
0.5 km s−1
1. How abundan is HCl ac oss he inne Galaxy?
2. Is he e widesp ead line o sigh abso p ion in he
Galac ic a ms?
3. Wha physical and exci a ion condi ions does HCl ace?
4. A e a ia ions o he 35Cl/37Cl a io a localized
phenomenon, o does a galac ic end exis ?
‣Is he iso opic a io linked o supe no a emnan s?
APEX 12m sub-mm elescope
a 5104 m, Llano de Chajnan o
HPBW:
10.1′ ′
HCl
37
HCl
35
co e s 2 x 7.9 GHz
a mosphe ic H O
abso p ion!
2
ypical wea he
condi ions o ou
obse a ions
Figu e C edi : Neu eld & Wol i e (2009)
Dashed lines: 10 imes highe CR ioniza ion a e
deepe
su ace
HCl aces
dense co es
Chemical e olu ion ac oss he dep hs o a cloud
HCl
and o some deg ee
anslucen gas
0
–2
A [mag]
–4
log (abundance/elemen al)
–6
0 2 4 6 8 10
A ypical HCl line p o ile in ou sample consis s o
1. a na ow co e componen
2. a b oad, o en o se ou low componen
70 80 130
0.00
0.25
1.00
2
3
4
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.25
0.50
0.75
1.00
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
G029.954–00.016
Tmb [K]
dN
dυ[cm−2
km s−1]
υLSR [km s−1]
CH3OCH3 (?)
& CH3CN (?)
ou low
wing
ou low
wing
υLSR [km s−1]
υsys
heo e ical
HFS line
in ensi y
624.977821 GHz625.918756 GHz
2
4
3
G029.954–00.016
0.50
0.75
90 100 110 120 70 80 13090 100 110 120
APEX 12m sub-mm elescope
hype ine s uc u e
(HFS) decon ol ed
column densi y p o ile
In summa y, 11 o he 28 a ge ed sou ces showed only emission line
p o iles (including one en a i e de ec ion).
17 had one o mo e addi ional abso p ion componen s, o en ende ing
analyses di icul .
F om hese obse a ions, we could de i e he iso opic a io in wo ways:
om he XCLASS line p o ile models, incl. sou ces wi h well sepa a ed, o
no abso p ion componen s
om he in eg a ed in ensi y a io, whe e we cu ou con aminan s and ha e
o disca d sou ces wi h abso p ion
line p o ile
modeled wi h
XCLASS
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
70 80 90 100 110 120 130
LSR [km s°1]
0.00
0.05
0.10
0.15
dN
d [cm°2
km s°1]
£1013
70 80 90 100 110 120 130
LSR [km s°1]
£1013
W43 MM1
0.15
Tmb [K]
dN
dυ[cm−2
km s−1]
3
υLSR [km s−1]
υLSR [km s−1]
70
80
130
90
100
110
120
70
80
130
90
100
110
120
W 43 MM-1
CH3OCH3 (?)
& CH3CN (?)
dominan
abso p ion
0.10
0.05
0.00
4
5
1
2
3
4
5
Tmb [K]
H35Cl (1°0) H37Cl (1°0)
°10 0 10 20 30 40 50
LSR [km s°1]
0.0
0.5
1.0
dN
d [cm°2
km s°1]
£1013
°10 0 10 20 30 40 50
LSR [km s°1]
£1013
HGAL 000.546–00.852
o se
abso p ion
υLSR [km s−1]
–10 05010 20 30 40
υLSR [km s−1]
–10 05010 20 30 40
HGAL 000.545–00.852
CH3OCH3 (?)
& CH3CN (?)
emission
om co e
Tmb [K]
dN
dυ[cm−2
km s−1]
1
1.0
0.5
0.0
4
5
2
3
4
6
8
10
Tmb [K]
SO+
H35Cl (1°0) H37Cl (1°0)
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
0
1
2
3
dN
d [cm°2
km s°1]
£1013
°70 °60 °50 °40 °30 °20 °10
LSR [km s°1]
£1013
IRAS 12326–6245
CH3OCH3 (?)
& CH3CN (?)
υLSR [km s−1]υLSR [km s−1]
–70 –60 –10–50 –40 –30 –20 –70 –60 –10–50 –40 –30 –20
IRAS 12326–6245
ou low
SO+
massi e
ou low
emission
om co e
3
Tmb [K]
dN
dυ[cm−2
km s−1]
4
2
1
0
6
10
8
The line p o iles owa d some a ge s
show massi e ou lows:
Some show o se abso p ion:
And some e en show
dominan abso p ion:
a cha ac e is ic
zigzag pa e n
HCl has been de ec ed in 27 massi e s a - o ming egions.
‣The obse ed emission o en aces s ong ou lows
‣Complex line p o iles (emission wi h abso p ion) ende s modeling
he spec al line p o iles di icul
We ind an a e age chlo ine iso opic a io o
[H35Cl]/[H37Cl] = 2.6 ± 0.8.
‣The a io shows no sys emic end wi h galac ocen ic
dis ance.
‣Chlo ine iso opic a ios ha e been obse ed o he i s ime in he
Galac ic cen e , whe e hey a e highe , bu s ill ag ee wi h
CCSN models (Maas & Pilachowski, 2021).
‣Cu en ly, i emains unclea whe he he a io is highe o a ge s
in he icini y o SNRs.
We plan o analyze he physical and exci a ion
condi ions aced by HCl.
Fo his, we a e explo ing HCl’s spa ial dis ibu ion,
especially in ou lows o disen angle bo h componen s:
‣Mapping HCl owa d IRAS 12326–6245 and
i s massi e ou low
RA (J2000)
Dec (J2000)
[K km s–1]
12h35m42s
39s
36s
33s
30s
–62°02'00"
03'00"
20"
40"
100
80
60
40
20
wo k in p og ess
Fi s look a he
HCl (1–0) map
ou low
Pho odissocia ion model p edic ions
o he abundances o chlo ine-bea ing
(and luo ine-bea ing) species ela i e
o he elemen al abundances ac oss he
dep hs o an in e s ella cloud
Chlo ine-bea ing molecules ha e diagnos ic p ope ies
due o chlo ine’s unique chemis y
‣Mos in e s ella chlo ine is con ained in ≤6 species
‣Chlo ine is p ima ily ionized (IPCl = 12.968 eV < IPH) and
highly eac i e
‣The chemical ne wo k is ini ialized by he exo he mic
(D0(HCl+) > D0(H2)) eac ion Cl+ + H2 → HCl+
Chemical ne wo k displaying
he mos ele an gas-phase
o ma ion and des uc ion pa hways
o chlo ine chemis y in he ISM.
Based on Fig. 3, Neu eld e al. (2021)
Neu eld & Wol i e (2009)
We used XCLASS (Mölle , End es & Schilke, 2017) o model he
obse ed line p o iles. XCLASS assumes LTE and op imizes a
numbe o sou ce pa ame e s pe componen . While we le column
densi y, iso opic a io and line wid h open, we cons ained
‣ he sou ce size, , ( e i ied wi h ATLASGAL),
‣ he o a ional empe a u e, T o = Tdus , ( om ATLASGAL),
‣and he eloci y o se , < 1 km s–1, o he co e componen .
- and he numbe o componen s ha e been de e mined
om H13CO (7–6), co e ed in he lowe sideband
-o CO iso opologues (Gianne i e al., 2014)
θs= 20′ ′
υoff
υLSR +
p edic ions o he
sola neighbo hood
om Galac ic chemical
e olu ion models
(Kobayashi e al., 2011)
R1
R2
