Dust in edge-on spiral galaxies from the J-band of the 2MASS Large Galaxy Atlas
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Dust in edge-on spiral galaxies from the J-band of the 2MASS Large Galaxy Atlas. Angelos Misiriotis (1) and Manolis Xilouris (2). (1) University of Crete, Department of physics (2) National observatory of Athens. Motivation (a case for “optical” detection of dust).

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Dust in edge-on spiral galaxies from the J-band of the 2MASS Large Galaxy Atlas

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Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Dust in edge-on spiral galaxies from the J-band of the 2MASS Large Galaxy Atlas

Angelos Misiriotis (1) and Manolis Xilouris (2)

(1) University of Crete, Department of physics

(2) National observatory of Athens


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Motivation

(a case for “optical” detection of dust)

  • Optical studies are coplementary to FIR observations

  • Require less exotic equipment

  • Take advantage of huge archaives

  • Constrain the emissivity


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Why edge-on ?

Image from the 2MASS L.G.A.

Jarrett T. H., Chester T., Cutri, R. Schneider, S. E. Huchra, J. P., 2003, AJ, 125, 525


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Why J-band ?

  • In the J Band (τ ~ 0.1)

  • The edge-on line of sight reaches the center

  • The dust lane is still visible

Figure from:

Bosma A., Byun Y., Freeman K. C. Athanassoula E., 1992, ApJ, 400, 21


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Why the 2MASS, Large Galaxy Atlas(*)?

  • Large homogenious sample

  • Easily available

  • Good pilot before spending months for deeper observations

Out of the LGA 28 edge-on galaxies were

selected for this study.

(*)Jarrett, T. H.; Chester, T.; Cutri, R.; Schneider, S. E.; Huchra, J. P.,

2003AJ....125..525J


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

The Model

  • A stellar bulge (de Vaucoulers)

Xilouris E. M., Byun Y. I., Kylafis N. D., Paleologou E. V., Papamastorakis, J.,

1999, A&A, 344, 868


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

The Model

  • A stellar bulge (de Vaucoulers)

  • A stellar exponential disk

Xilouris E. M., Byun Y. I., Kylafis N. D., Paleologou E. V., Papamastorakis, J.,

1999, A&A, 344, 868


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

The Model

  • A stellar bulge (de Vaucoulers)

  • A stellar exponential disk

  • An exponential dust disk

Xilouris E. M., Byun Y. I., Kylafis N. D., Paleologou E. V., Papamastorakis, J.,

1999, A&A, 344, 868


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Textbook Cases

(7/28 galaxies )

Observation

Model


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Passable Cases

(8/28 galaxies )


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Impossible Cases

(5+8/28)

Which leaves us with 15/28 galaxies to draw some results on the dust properties.


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Results

Optical depth as a function of MK


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Results

Optical depth as a function of dust mass


Dust in edge on spiral galaxies from the j band of the 2mass large galaxy atlas

Conclusions

J-Band is ideal for optical studies of dust in edge-on galaxies provided a high resolution.

Larger spirals exhibit higher face-on optical depth.

There might be a threshold of the optical depth in normal spiral galaxies.


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