Документ взят из кэша поисковой машины. Адрес оригинального документа : http://jet.sao.ru/hq/katya/InterCloud/krelowski2.pdf Дата изменения: Wed Feb 24 16:35:59 2010 Дата индексирования: Tue Oct 2 01:17:37 2012 Кодировка: Поисковые слова: п п п п п п п п п п п п п п п п р п р п р п р п р п р п р п р п р п р п

Diffuse interstellar bands vs. rotational temperatures of simple molecular species
Jacek Krelowski
Centrum Astronomii UMK jacek@astri.uni.torun.pl


Collaborators: Gazinur A. Galazutdinov Faig A. Musaev Tomasz Weselak Mirek R. Schmidt Piotr Gnaciski Arkadiy Bondar
Bohyunsan Optical Astronomy Observatory, Jacheon, YoungChun, KyungPook, 770-820, South Korea Special Astrophysical Observatory, Nizhnyi Arkhyz, Russia University of Bydgoszcz, Poland

Center for Astronomy, Polish Academy of Sciences, Toru, Poland Institute of Theoretical Physics and Astrophysics, Gdask University, Poland International Center for Astronomical and Medico-Ecological Research Russia-Ukraine


Absorption spectral features originated in interstellar clouds
Atomic lines from ground levels (known since 1904)
CaII, NaI, KI, CaI and LiI (vis.) Others ­ far-UV (Copernicus, IUE, HST)

Features of simple molecules (known since 1937)
Polar species: CH, CH+, CN, CO Homonuclear ones: H2, C2, C3

Diffuse interstellar bands (known since 1922)
Unidentified; Proposed carriers: carbon chains, PAHs, fulleranes


Radial velocity of CH+ can be different than those of other species
1.6

RbI 7800A*3 CN 3875A

Relative intensity

1.4

CH 3886A CH 4300A/2

1.2

FeI 3720A CH 3957A
1.0
+

CH 4232A
HD152932 ESO UVES
-60 -30 0 30 60

+

Radial velocity


Diffuse bands (strong and weak) may be of different origin(s)
5780
5772 5775

5797

HD147165

5795

1.02

Relative intensity

5763

5766

5769

5785

HD179406

5793

0.96

ESO/HARPS spectrograph
0.90

R=115,000
5770 5780 5790 5800

Wavelength (A)


Standard DIB wavelengths(radial velocities according to CH and KI) in HD179406

DIB 6196

DIB 4964

1.17

Relative intensity

FeI 3860 A

CN 3874 A

1.08
CH 3886 A

KI 4044 A

0.99 -100

CH+ 3957 A

-50

0

50

100

Radial velocity (km/s)


High precision HARPS spectrum suggests that DIBs belong to at least two"families"

4
DIB 4964 A

Normalized intensity

3
DIB 6196 A

2

CH 4300 A

1

CaII 3933 A

0

HD152233 HARPS
-100 -50 0 50 100 150

Radial velocity (km/s)


Diffuse band 6196 seemingly shares Doppler shift with CH+...
1.12
DIB 6196

CH+ 3957 A

Relative intensity

1.04

DIB 4964

CH 3886 A

0.96

HD 151932 UVES R=80,000 - 110,000
-80 0 80

Radial velocity (km/s)


... even when it is very small

1.0

0.9

Relative intensity

0.8

DIB 6196
+

CH 3886A

0.7

CH 3957A

0.6 -30 -15 0

HD147889 UVES - cold colors HARPS - warm colors
15 30

Radial velocity (km/s)


Comment
· It is of basic importance to establish spatial correlations of DIB carriers and well known atoms (ions) and molecules (their ions) · Profiles of interstellar features depend on both: physical parameters of interstellar clouds and distributions of radial velocities along sightlines


Difficult choice of a sample where CH+ line is narrow, free of Doppler splitting and shares radial velocity with other molecules

0.9

HD 148184

Normalized intensity

0.6

HD 147889 HD 169454 HD 163800 HD 179406

0.3

0.0

CH 4232A UVES; R= 80, 000
-20 -10 0 10

+

Radial velocity (km/s)


DIB broadening with Trot of C2; note also substructures
HD147889

DIB 6196
0.99

HD169454

R10

R12

Relative intensity

1.05

HD147889

HD169454

0.98 R 6
R4 Q
4

P2 Q
6

Q

Q
8

0.96
10

0.91

R2

R0

C2 Phillips (2,0) band UVES R=110,000

0.93 6195.0 6195.7

Q

UVES R=110,000

2

8760

8770

8780

6196.4

6197.1

Wavelength (A)


Strength ratio of Q6/Q2 transitions in C2 indicates growth of Trot from 179406 to 148184
4

HD 148184

Normalized intensity

3

HD 147889

2

HD 163800
1

R6
0

R

4

R2
8754

R0 Q
8760
2

P2 Q
4

HD 179406

Q

Q8 P

4

6

8766

8772

Wavelength (A)


Diffuse interstellar band 6196 seen in the same, high quality spectra
1.2

D I B 6194. 5

D I B 6196

Normalized intensity

0.8

HD 179406 HD 163800 HD 147889 HD 148184

0.4

0.0

HARPS; R=115,000
6194.7 6195.6 6196.5

Wavelength (A)


Here red wings overlap each other
D I B 6194. 5 D I B 6196

Normalized intensity

0.8

HD 179406 HD 163800 HD 147889 HD 148184
0.4

0.0

HARPS; R=115,000
6195 6196 6197

6194

Wavelength (A)


Growing FWHM of 6196 is accompanied with the intensity growth of the neighbour 6203 DIB
1.0

D I B 6203

HD 179406

Normalized intensity

HD 163800
0.5

HD 147889 HD 148184

0.0

D I B 6196
6196 6200

HARPS; R=115,000
6 20 4 6 20 8

Wavelength (A)


Physically caused variations of the 6196 profile (spectra from ESO, R=220,000, S/N~1000)


Physical broadening of diffuse band profiles CES/3.6m ESO R=220,000; profiles normalized

1.00

0.95

DB 6196 I DB 6614 I H 147165 B III E(BV 0.34 D 1 - )=

Normalized intensity

0.90

0.85

H 179406 B V E(BV=0.31 D 3 -)

0.80

K 7699 A I
-90 -60 -30 0 30 60 90

Radial velocity


Rotational temperature of C2 seems to be correlated with that of C3
1.04

HD 148184
1.02

Relative intensity

HD 147889

HD 163800
1.00

HD 179406
0.98

KI
0.96

C3

KI
4044 4046 4048 4050 4052 4054

Wavelength (A)


Comment
· Rotational temperatures of simple carbon species (C2 i C3) seem to be correlated · Molecules C2 i C3 are the only species, available to ground-based observations, for which the observed Trot's are evidently different · 6196 DIB profile gets broader while Trot gets higher


Profile of the 6614 DIB, well correlated with 6196, changes the shape with Trot of C2 i C3
D I B 6614
HD 148184

Normalized intensity

2

HD 147889

HD 163800
1

HD 179406

0 6612 6613 6614 6615

Wavelength (A)


Trot(179406) < Trot(147889)...

DIB 6614
Normalized intensity

0.8

HD179406 HD147889
0.4

0.0 6612 6614

HARPS; R=115,000
6616

Wavelength (A)


Profile of 5797 DIB behaves in a fashion similar to that of 6196
DIB 5793
HD179406

DIB 5797

Normalized intensity

2

HD163800

HD147889

1
HD148184

0

ESO HARPS R=115,000
5793 57 96 5799

Wavelength(A)


Profiles of the DIBs: 6196 i 6379 change in unison (spectra from Gecko CFHT)


The same effects seen in high quality spectra from ESO HARPS spectrograph
DIB6376 DIB6379

Normalized intensity

0.8

HD179406 HD147165

0.4

0.0

HARPS; R=115,000
6375 6378 6381

Wavelength(A)


6379 DIB profile behaves in our sample as that of 6196
DIB 6376
HD179406

DIB 6379

Normalized intensity

2

HD163800

HD147889

1
HD148184

0

ESO HARPS R=115,000
6376 6378 6380

Wavelength(A)


6196 profile broadening is not caused by Doppler splitting ­ absent in CH lines

1.00

Relative intensity

0.96

DIB 6196
0.92

HD179406 HD147889 HARPS R=115,000
0.88 -40 -20

CH 4300
0 20 40

Radial velocity (km/s)


Substructures are not equally spaced in all spectra which is the argument against isotope shift
CH
0.96

Normalized intensity

DIB 6379
0.88

HD147889
0.80

HD179406 HARPS R=115,000
-50 -25 0 25 50

Radial velocity (km/s)


The same is true in the case of 5797 DIB (5796.97)
CH

0.99

Normalized intensity

0.90

DIB 5797

HD147889
0.81

HD179406 HARPS R=115,000
-30 0 30 60 90

Radial velocity (km/s)


Broad 5780 DIB also changes profile together with Trot
CH
0.99

5776 Normalized intensity

5785

0.90

DIB 5780

HD147889
0.81

HD179406 HARPS R=115,000
-200 -100 0 100 200 300

Radial velocity (km/s)


4964 DIB profile remains unchanged...

CH
0.96

Normalized intensity

DIB 4964
0.88

HD147889 HD179406
0.80

HARPS R=115,000
-50 -25 0 25 50

Radial velocity (km/s)


...as well as other blue DIBs...

CH
0.96

DIB?

Normalized intensity

DIB 4735

0.88

DIB 4726

HD147889
0.80

HD179406 HARPS R=115,000
-200 0 200 400 600

Radial velocity (km/s)


...including very broad 4430 as far as contaminating stelar lines permit to judge
CH
0.99

Normalized intensity

0.90

DIB 4430
0.81

HD147889 HD179406 HARPS R=115,000

-1000

-500

0

500

1000

1500

Radial velocity (km/s)


Extremely high rotational C2 temperature toward AE Aur (BOES vs. UVES)
1.05

HD 34078

Relative intensity

1.02

HD179406

0.99
P2 Q6 Q8 Q10 P6

Q12

R0

0.96

Q2

Q4

ESO/UVES R=110,000
8770 8780 8790

8760

Wavelength(A)


The same effects for C3 (Adamkovics & al.. 2003)


DIB 5797 blue-shifted and broadened in the spectrum of AE Aur
1.00

Relative intensity

0.96

HD34078 Maestro HD34078 BOES

0.92

HD179406 HARPS
5795 5796 5797 5798 5799

Wavelength(A)


The same blue-shift confirmed by BOES spectrograph (Per vs. AE Aur).
HD 24398

DB 5797 I
0.99

Normalized intensity

HD 34078

0.96

Vr = 0 acc. to KI 7699 A

0.93

BOES, R=90,000
5796.0 5797.5 5799.0

Wavelength (A)


Stellar and interstellar features identical in HD34078 spectra from two instruments
1.00

AE Aur HD34078 BOAO Boes R=90,000
Relative intensity
0.96

Terskol Maestro R=120,000

DIB 5797
0.92

CIV stellar
5795.0 5797.5 5800.0 5802.5

Wavelength (A)


DIB 6379 in AE Aur is also blue-shifted and attenuated
1.00

DIB 6376

DIB 6379

Relative intensity

0.99

HD34078 BOES

0.98

0.97

HD179406 HARPS 3 times shrinked

6374

6376

6378
Wavelength(A)

63 80


Conclusions
· Rotational temperatures of simple, linear carbon species may be seriously different; a majority of cases fills a rather narrow range · Profiles of some of the diffuse bands vary also with Trot which may suggest their carriers are also centrosymmentric molecules