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