Catalogue of Herschel-PACS spectroscopic observations of ... · jet-disc contribution Extended [OI] emission T Tau • emission. Compare continuum-to-line ratio in the • • Extended

P. Riviere-Marichalar

Catalogue of Herschel-PACS spectroscopicobservations of Young Stellar Objects: the

jet-disc contribution

Catalogue of Herschel-PACS spectroscopic

observations of Young Stellar Objects: the jet-disc

contribution


ALMA/Herschel Archival Workshop, Garching, April 2015

1 / 15




Protoplanetary discs

• Discs of gas and dust surrounding young stars. Birthplace for

planets• Dust: IR-excess.

◮ SED modelling◮ Scattered light◮ Resolved thermal emission

• Gas: spectroscopy at many wavelengths

1.0 10.0 100.0 1000.

10−16

10−14

10−12

10.0 20.5.

10−13

2

λ (µm)

λ.F

λ (W

.m−2

)

SED: dustPinte+ (2008)

Scattered lightimaging: dustPinte+ (2008)

Continuum thermalemission: dust

Williams and Cieza (2009)

Introduction 2 / 15




Protoplanetary discs

• Discs of gas and dust surrounding young stars. Birthplace for

planets• Dust: IR-excess.

◮ SED modelling◮ Scattered light◮ Resolved thermal emission

• Gas: spectroscopy at many wavelengths

Sub-mm spectroscopy: gasWilliams and Cieza (2009)

Near-IR spectroscopy: gasSalyk+ (2008)

Introduction 2 / 15




PACS spectroscopy

• Far-IR spectroscopy in the 50-200 µm• Two modes: line- and range-scan• Emission from species such as: O, H2O, CH

+, OH, [CII]• PACS IFU: spatial information• Many PACS programs to observe gas in protoplanetary discs:

GASPS, DIGIT, WISH, ...• More than 300 YSOs observed with PACS spectroscopy

Introduction 3 / 15




Observations of [OI]

• The most frequent far-IR line emission from discs

• Brightest far-IR line in discs (Gorti & Hollenbach 2008)

Observations of YSOs at 63 µm 4 / 15




...and water!

• 24% of gas-rich discs show water emission (Riviere-Marichalar+

2012)

63.0 63.1 63.2 63.3 63.4λ (µm)

0.5

1.0

1.5

2.0

2.5

3.0

Flux (Jy)

63.0 63.1 63.2 63.3 63.4λ (µm)

0

100

200

300

400

500

600

Flux (Jy)

63.0 63.1 63.2 63.3 63.4λ (µm)

60

65

70

75

80

85

90

95

100

Flux (Jy)

63.0 63.1 63.2 63.3 63.4λ (µm)

0.2

0.4

0.6

0.8

1.0

1.2

1.4

Flux (Jy)





[OI] emission: the disc-jet contribution

Howard+ 2013, Riviere-Marichalar+ 2015

• YSOs with outflows (or jets) show higher [OI] for the same flux at 70 µm• The difference is more pronounced for bright continuum sources• Both the jet and the disc contribute to [OI] emission• The line flux is upper limit to disc emission





Extended [OI] emission

T Tau

62.963.063.163.263.363.463.5−1

012345678

Flux (

Jy)

00

62.963.063.163.263.363.463.505

10152025303540

01

62.963.063.163.263.363.463.50

5

10

15

2002

62.963.063.163.263.363.463.5

0

2

4

6

8

03

62.963.063.163.263.363.463.5−1.0−0.5

0.00.51.01.52.02.53.0

04

62.963.063.163.263.363.463.502468

10121416

Flux (

Jy)

10

62.963.063.163.263.363.463.50

50

100

150

20011

62.963.063.163.263.363.463.50

20

40

60

80

100

120

14012

62.963.063.163.263.363.463.502468

1012141618

13

62.963.063.163.263.363.463.5−1.0−0.5

0.00.51.01.52.02.53.03.5

14

62.963.063.163.263.363.463.50

2

4

6

8

10

12

14

Flux (

Jy)

20

62.963.063.163.263.363.463.50

20

40

60

80

100

120

14021

62.963.063.163.263.363.463.550

100150200250300350400450

22

62.963.063.163.263.363.463.5−5

0

5

10

15

2023

62.963.063.163.263.363.463.5−1

0

1

2

3

4

524

62.963.063.163.263.363.463.5−1

0

1

2

3

4

5

6

Flux (

Jy)

30

62.963.063.163.263.363.463.5−2

02468

10121416

31

62.963.063.163.263.363.463.50

20

40

60

80

10032

62.963.063.163.263.363.463.5−2

02468

101214

33

62.963.063.163.263.363.463.5−4

−2

0

2

4

6

8

1034

62.963.063.163.263.363.463.5

λ(µm)

−2

−1

0

1

2

3

Flux (

Jy)

40

62.963.063.163.263.363.463.5

λ(µm)

−1

0

1

2

3

4

541

62.963.063.163.263.363.463.5

λ(µm)

−5

0

5

10

15

20

2542

62.963.063.163.263.363.463.5

λ(µm)

−2

0

2

4

6

8

1043

62.963.063.163.263.363.463.5

λ(µm)

−2−1

0123456

44

• Extended emission along the

jet direction

• Podio+ (2012): test extended

emission. Compare

continuum-to-line ratio in the

24 spaxels with that of the

central one

• Podio+ (2012): "The extended

atomic emission may be

produced by fast J-shocks"






DG TauA

-20 -10 0 10 20 30RA offset (arcsec)

-20

-10

0

10

20

Dec

off

set (

arcs

ec)

DG Tau A: [SII] 6731 A + [OI] 63.2µm

05

10152025

Flux

(Jy

)

(0,0) -0.04 Jy

2.0e-17 W/m2

8.05

(0,1) 0.18 Jy

2.5e-17 W/m2

11.26

(0,2) 0.16 Jy

(0,3) 0.05 Jy

(0,4) -0.57 Jy

05

10152025

Flux

(Jy

)

2.0e-17 W/m2 8.33

(1,0) 0.17 Jy

4.3e-16 W/m2

5.68

(1,1) 5.48 Jy

1.2e-16 W/m2

8.49

(1,2) 1.05 Jy

1.5e-17 W/m2

> 100

(1,3) 0.01 Jy

(1,4) -0.11 Jy

2.3e-17 W/m2

9.28

(2,0) 0.18 Jy

4.2e-16 W/m2

7.86

(2,1) 3.82 Jy

4.4e-16 W/m2

8.26

(2,2) 3.88 Jy

2.5e-17 W/m2

> 100

(2,3) 0.01 Jy

(2,4) -0.04 Jy

1.4e-17 W/m2

10.86

(3,0) 0.09 Jy

3.1e-17 W/m2

21.89

(3,1) 0.10 Jy

1.0e-16 W/m2

13.91

(3,2) 0.54 Jy

1.4e-17 W/m2

5.53

(3,3) -0.18 Jy

(3,4) -0.18 Jy

(4,0) 0.09 Jy

1.2e-17 W/m2

20.41

(4,1) 0.04 Jy

63.12 63.18 63.24λ (µm)

2.0e-17 W/m2

8.20

(4,2) 0.18 Jy

63.12 63.18 63.24λ (µm)

(4,3) 0.04 Jy

63.12 63.18 63.24λ (µm)

(4,4) 0.00 Jy

(Podio+ 2012)


jet direction


emission. Compare



central one









DK Cha

(Riviere-Marichalar+ 2015)


jet direction


emission. Compare



central one








[OI]: multiple components

• DK Cha: multiple componentsobserved (Riviere-Marichalar+2015)

◮ Low-velocity (-51–52km/s,

rest-frame?) component

(disc?, stellar wind?)◮ High-velocity, red- (126–222

km/s) and blue-shifted (-70 –

-177 km/s) components(jet?)

• Spatial distribution of the

components

63.10 63.12 63.14 63.16 63.18 63.20 63.22 63.24

0

20

40

60

80

Fν(Jy)

1-Gaussian fit

63.10 63.12 63.14 63.16 63.18 63.20 63.22 63.24

0

20

40

60

80

Fν(Jy)

2-Gaussians fit

63.10 63.12 63.14 63.16 63.18 63.20 63.22 63.24λ(µm)

0

20

40

60

80

Fν(Jy)

3-Gaussians fit





[OI]: multiple components

• DK Cha: multiple componentsobserved (Riviere-Marichalar+2015)

◮ Low-velocity (-51–52km/s,rest-frame?) component

(disc?, stellar wind?)◮ High-velocity, red- (126–222

km/s) and blue-shifted (-70 –

-177 km/s) components

(jet?)

• Spatial distribution of the

components

(Riviere-Marichalar+ 2015)





Other lines?

(Alonso & Riviere-Marichalar, to be submitted)





• ∼ 330 observations of YSOs at 63 µm: [OI] and o-H2O◮ Ages: 3–30 Myr (plus some old DD)◮ Class 0, I, II, III, transition discs, debris discs◮ Spectral types A to M

• Test extended emission• Understand jet and disc contribution• Evolutionary timescales• Future prospects: extend to range spectroscopy: CO, OH, H2O,

[CII],...

Catalogue of observations at 63 µm 10 / 15






[CII],...

10-17 10-16 10-15 10-14 10-13

F[OI] (erg/cm2 /s/Å)

10-17

10-16

10-15

10-14

10-13

F[O

I][3x3] (erg/

cm2/s/Å

)







[CII],...

0 2 4 6 8 10 12

Age (Myr)

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

Fraction

0.84×e−t/4.2 +0.10UpSco

Taurus Oph

Lupus

EtaCha

ChaII

Cha





OI spatial distributions

65.5022 65.4996 65.496 65.4943 65.4917RA

19.530

19.533

19.535

19.538

19.541

Dec

T_Tau

0.0

0.9

1.8

2.7

3.6

4.5

5.4

1e−15

67.9188 67.9161 67.9135 67.9109 67.9083RA

18.230

18.232

18.235

18.237

Dec

XZ_Tau-1

0.0

0.6

1.2

1.8

2.4

3.0

3.6

1e−16

193.324 193.322 193.3194 193.316 193.314RA

-77.124

-77.122

-77.119

-77.116

-77.114

Dec

ChaII-J12531723-7707107

0.00

0.24

0.48

0.72

0.96

1.20

1.44

1e−15

65.5022 65.4996 65.496 65.4943 65.4917RA

19.530

19.533

19.535

19.538

19.541

Dec

T_Tau

0.00000000

0.00000018

0.00000036

0.00000054

0.00000072

0.00000090

0.00000108

67.9188 67.9161 67.9135 67.9109 67.9083RA

18.230

18.232

18.235

18.237

Dec

XZ_Tau-1

−0.00000108

−0.00000090

−0.00000072

−0.00000054

−0.00000036

−0.00000018

0.00000000

193.324 193.322 193.3194 193.316 193.314RA

-77.124

-77.122

-77.119

-77.116

-77.114

Dec

ChaII-J12531723-7707107

0.0

0.4

0.8

1.2

1.6

2.0

2.4

2.8

3.21e−7





H2O spatial distributions

65.5022 65.4996 65.496 65.4943 65.4917RA

19.530

19.533

19.535

19.538

19.541

Dec

T_Tau

−0.3

0.0

0.3

0.6

0.9

1.2

1.5

1.8

2.11e−16

67.9188 67.9161 67.9135 67.9109 67.9083RA

18.230

18.232

18.235

18.237

Dec

XZ_Tau-1

−1.8

−0.9

0.0

0.9

1.8

2.7

3.6

1e−17

193.324 193.322 193.3194 193.316 193.314RA

-77.124

-77.122

-77.119

-77.116

-77.114

Dec

ChaII-J12531723-7707107

−2.4

−2.0

−1.6

−1.2

−0.8

−0.4

0.0

0.4

1e−17

65.5022 65.4996 65.496 65.4943 65.4917RA

19.530

19.533

19.535

19.538

19.541

Dec

T_Tau

−9.0

−7.5

−6.0

−4.5

−3.0

−1.5

0.0

1.51e−17

67.9188 67.9161 67.9135 67.9109 67.9083RA

18.230

18.232

18.235

18.237

Dec

XZ_Tau-1

0.0

0.3

0.6

0.9

1.2

1.5

1.8

2.1

1e−16

193.324 193.322 193.3194 193.316 193.314RA

-77.124

-77.122

-77.119

-77.116

-77.114

Dec

ChaII-J12531723-7707107

−2.1

−1.8

−1.5

−1.2

−0.9

−0.6

−0.3

0.0

0.3

0.61e−17





A global picture: many parameters, manyobservations

• SED: Mdust, ǫ, amin–rin, p...

• Thermal image, scattered lightimage: Rin, Rout, ǫ

◮ Need for high spatial

resolution to access innerdisc: ALMA!, Sphere...

• Spectroscopy: gascomposition and dynamics, β,fUV,...

◮ Gas and dust can have

different spatial distribution:

ALMA! to trace gas VS dust

• Polarimetry: dust composition

and size

1.0 10.0 100.0 1000.

10−16

10−14

10−12

10.0 20.5.

10−13

2

λ (µm)

λ.F

λ (W

.m−2

)

Pinte+ (2008)















and size

HD 21997 - ALMA 886µm

4 2 0 -2 -4RA offset [arcsec]

-4

-2

0

2

4

DE

C o

ffse

t [a

rcse

c]

50 AU

-0.20

0.00

0.20

0.41

0.61

I ν [

mJy b

eam

-1]

a

Moór + (2013)















and size

arcseconds East

arc

seconds N

ort

h

0.99 µm-1-0.500.51

-1

-0.5

0

0.5

1

SN

RE

-5

0

5

10

15

20

Rodigas+ (2015)















and size

-4 -2 0 2 4 6 8vLSR (km s

-1)

0.0

0.1

0.2

0.3

0.4

0.5

0.6

SC

O (

Jy)

12CO(3-2)12CO(2-1)13CO(3-2)13CO(2-1)

C18O(2-1)

Kóspál+ (2013)















and size

-1

0

1

2

3

vL

SR (k

m s

-1)

3 2 1 0 -1 -2RA offset (arcsec)

-3

-2

-1

0

1

2

DE

C o

ffse

t (a

rcse

c)

12CO (2-1)

Kóspál+ (2013)





• Catalogue of spectroscopic observations of > 330 YSO’s

• Disentangle jet and disc contribution to [OI] emission

• Complement with other lines to model the gas content

Summary 14 / 15




Thanks for your attention

Summary 15 / 15

IntroductionObservations of YSOs at 63 mCatalogue of observations at 63 mSummary

Documents

Catalogue of Herschel-PACS spectroscopic observations of ... · jet-disc contribution Extended [OI] emission T Tau • emission. Compare continuum-to-line ratio in the • • Extended