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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. 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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slide1

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

slide2

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
slide3

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

slide4

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

slide5

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

slide6

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

slide7

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

slide8

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

slide9

Textbook Cases

(7/28 galaxies )

Observation

Model

slide10

Passable Cases

(8/28 galaxies )

slide11

Impossible Cases

(5+8/28)

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

slide12

Results

Optical depth as a function of MK

slide13

Results

Optical depth as a function of dust mass

slide14

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.