IntroData
Analysis
The Survey of Lines in M31 (SLIM):Investigating the Origins of [CII] Emission
Maria Kapala
K. Sandstrom, B. Groves, K. Croxall, J. Dalcanton, K. Gordon, O. Krause,
K. Kreckel, A. Lewis, H. W. Rix, E. Schinnerer, F. Walter, D. Weisz
Phases of the ISM, July 31st
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Outline
1 Intro
2 DataSLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
3 AnalysisCII from SF regionsStellar populations heating ISMFar-IR line de�cit
4 Conclusions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Motivation: use [CII] 158 µm emission line
strong
easy to observe even in high z
Potentially can be used to
estimate SFR
probe some of the ISM physicalconditions
Colbert et al. 1998
Walter et al. 2009
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Motivation: use [CII] 158 µm emission line
strong
easy to observe even in high z
Potentially can be used to
estimate SFR
probe some of the ISM physicalconditions
Colbert et al. 1998
Walter et al. 2009
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Motivation: use [CII] 158 µm emission line
strong
easy to observe even in high z
Potentially can be used to
estimate SFR
probe some of the ISM physicalconditions
Colbert et al. 1998
Walter et al. 2009
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Issue: [CII] 158 µm emission from multiple ISM phases
CNM(cold neutral medium)
WNM(warm neutral medium)
WIM(warm ioinized medium)
PDRs(photodissotiation regions)
credit: Diane Cormier
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Issue: [CII] 158 µm emission from multiple ISM phases
CNM(cold neutral medium)
WNM(warm neutral medium)
WIM(warm ioinized medium)
PDRs(photodissotiation regions)
credit: Diane Cormier
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Issue: [CII] 158 µm emission from multiple ISM phases
CNM(cold neutral medium)
WNM(warm neutral medium)
WIM(warm ioinized medium)
PDRs(photodissotiation regions)
credit: Diane Cormier
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Issue: [CII] 158 µm emission from multiple ISM phases
CNM(cold neutral medium)
WNM(warm neutral medium)
WIM(warm ioinized medium)
PDRs(photodissotiation regions)
credit: Diane Cormier
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Issue: [CII] 158 µm emission from multiple ISM phases
CNM(cold neutral medium)
WNM(warm neutral medium)
WIM(warm ioinized medium)
PDRs(photodissotiation regions)
credit: Diane Cormier
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Solution: pick Andromeda
10'
N
E
2.3 kpc10’
PACS70PACS100SPIRE250
M31 (Andromeda)
Groves et al. (2012)
proximity → resolution
external view → no LOS confusionlarge, star-forming , metal-rich, L∗ galaxy
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Solution: pick Andromeda
10'
N
E
2.3 kpc10’
PACS70PACS100SPIRE250
M31 (Andromeda)
Groves et al. (2012)
proximity → resolutionexternal view → no LOS confusion
large, star-forming , metal-rich, L∗ galaxy
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Solution: pick Andromeda
10'
N
E
2.3 kpc10’
PACS70PACS100SPIRE250
M31 (Andromeda)
Groves et al. (2012)
proximity → resolutionexternal view → no LOS confusionlarge, star-forming , metal-rich, L∗ galaxy
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Large amount of ancillary data
Herschel (spectroscopy and photometry)70− 500µm at a spatial resolution down to ∼ 45 pc at 160µm
Calar Alto (PPAK) - optical IFS
HST (Pan-chromatic Hubble Andromeda Treasury survey)properties of individual stars > A0
and others
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Large amount of ancillary data
Herschel (spectroscopy and photometry)70− 500µm at a spatial resolution down to ∼ 45 pc at 160µm
Calar Alto (PPAK) - optical IFS
HST (Pan-chromatic Hubble Andromeda Treasury survey)properties of individual stars > A0
and others
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Large amount of ancillary data
Herschel (spectroscopy and photometry)70− 500µm at a spatial resolution down to ∼ 45 pc at 160µm
Calar Alto (PPAK) - optical IFS
HST (Pan-chromatic Hubble Andromeda Treasury survey)properties of individual stars > A0
and others
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
SLIM coverage
Andromeda galaxy
Herschel PACS regions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Herschel [CII] maps
PI Karin Sandstrom
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PPAK IFS data in �eld 1
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PPAK IFS data in �eld 1
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PPAK IFS data in �eld 1
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PPAK Hα
PI Karin Sandstrom
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PHAT coverage
Andromeda galaxy
PHAT footprint (blue), current stellar catalogs coverage (red) andHerschel regions (white boxes)
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
PHAT stellar SEDs �ts
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Stellar SED in �eld 3
103 104
λ [nm]
10-11
10-10
10-9
10-8
νFν
[erg/scm
2]
UVatt
Stellar SED unred
Stellar SED
stellar catalogs: K. Gordon
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
SLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
Stellar UVatt in �eld 3
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
ISM tracers in �eld 3
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
ISM tracers in �eld 3
Contours: Hα
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
[CII] emission from SF regions in �eld 2
HII regions - Azimlu et al. 2011
level: 3.25 · 10−155.3% from 1.2% area
level: 6 · 10−1637% from 15% area
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
[CII] emission from SF regions in �eld 2
HII regions - Azimlu et al. 2011
level: 3.25 · 10−155.3% from 1.2% area
level: 6 · 10−1637% from 15% area
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
[CII] emission from SF regions in �eld 2
HII regions - Azimlu et al. 2011
level: 3.25 · 10−155.3% from 1.2% area
level: 6 · 10−1637% from 15% area
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
CII & SFR correlation in �eld 3
10-2 10-1
SFRHα+24µm [M¯ yr−1 kpc−2 ]
10-5
10-4I C
II[ergs−
1cm
−2Sr−
1]
slope = 0.86
< SFR >= 0.023 M� yr−1 kpc−2 SFR formula: Calzetti et al. 2007
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
ISM tracers in �eld 3
Contours: UVatt
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
Stellar populations UV input to ISM in �eld 3
MB > 20M¯
34%
8M¯< MB
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
35%
58%59%
34%
65%
24%
This demonstrates that on ∼ kpc scales in Andromeda,massive B stars dominate the UV �eld as in the solar neighborhood.
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
ISM tracers in �eld 3
Contours: [CII]
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
No far-IR line de�cit
(O/H)/(O/H)� = 0.77, 0.94, 0.99, 0.98, 1.25
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
No far-IR line de�cit
(O/H)/(O/H)� = 0.77, 0.94, 0.99, 0.98, 1.25
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
No far-IR line de�cit
(O/H)/(O/H)� = 0.77, 0.94, 0.99, 0.98, 1.25
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
CII from SF regionsStellar populations heating ISMFar-IR line de�cit
No far-IR line de�cit
(O/H)/(O/H)� = 0.77, 0.94, 0.99, 0.98, 1.25
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Conclusions
[CII] correlates well with Hα emission, up to certain point
signi�cant amount of [CII] is coming from outside the SFregions → using [CII] to trace the massive SFR, one must takeinto account the contribution toISM gas heating by older stellar populations
on kpc scales UV radiation �eld (even in SF regions) aredominated by B stars
on 50 pc scales SF regions of M31do not show a �far-IR line de�cit� even in regions of warm dust
Not entire [CII] comes from SF regions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Conclusions
[CII] correlates well with Hα emission, up to certain point
signi�cant amount of [CII] is coming from outside the SFregions → using [CII] to trace the massive SFR, one must takeinto account the contribution toISM gas heating by older stellar populations
on kpc scales UV radiation �eld (even in SF regions) aredominated by B stars
on 50 pc scales SF regions of M31do not show a �far-IR line de�cit� even in regions of warm dust
Not entire [CII] comes from SF regions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Conclusions
[CII] correlates well with Hα emission, up to certain point
signi�cant amount of [CII] is coming from outside the SFregions → using [CII] to trace the massive SFR, one must takeinto account the contribution toISM gas heating by older stellar populations
on kpc scales UV radiation �eld (even in SF regions) aredominated by B stars
on 50 pc scales SF regions of M31do not show a �far-IR line de�cit� even in regions of warm dust
Not entire [CII] comes from SF regions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Conclusions
[CII] correlates well with Hα emission, up to certain point
signi�cant amount of [CII] is coming from outside the SFregions → using [CII] to trace the massive SFR, one must takeinto account the contribution toISM gas heating by older stellar populations
on kpc scales UV radiation �eld (even in SF regions) aredominated by B stars
on 50 pc scales SF regions of M31do not show a �far-IR line de�cit� even in regions of warm dust
Not entire [CII] comes from SF regions
Maria Kapala The Survey of Lines in M31 (SLIM)
IntroData
Analysis
Conclusions
[CII] correlates well with Hα emission, up to certain point
signi�cant amount of [CII] is coming from outside the SFregions → using [CII] to trace the massive SFR, one must takeinto account the contribution toISM gas heating by older stellar populations
on kpc scales UV radiation �eld (even in SF regions) aredominated by B stars
on 50 pc scales SF regions of M31do not show a �far-IR line de�cit� even in regions of warm dust
Not entire [CII] comes from SF regionsMaria Kapala The Survey of Lines in M31 (SLIM)
IntroDataSLIM - Survey of Lines in M31PHAT - Pan-chromatic Hubble Andromeda Treasury
AnalysisCII from SF regionsStellar populations heating ISMFar-IR line deficit