M82 — Tilt and Warp of its Principal Plane

Notni, P.; Bronkalla, W.

doi:10.1007/978-94-009-7075-5_17

Cited by 8 publications

(4 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Comparing the sum of the HI and H 2 column densities with the X-ray absorbing columns shows that the northern part of the disk of M 82 points toward the observer (Fig. 1), in agreement with reddening and polarization observations (Notni & Bronkalla 1983;Chesterman & Pallister 1980). A Galactic XeD of 1.6 x 10 20 cm-2 (Kkms-1 ) -1 (Hunter et al 1997) appears to overestimate the X-ray absorbing columns.…”

Section: Xeo Determination In M 82supporting

confidence: 81%

The M82 Outflow: X-rays as a Probe for Neutral Disk Gas

Ott

Walter²,

Kerp³

2004

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

Abstract. We present an analysis of X-ray absorption in the nearby starburst galaxy M 82. The X-ray attenuating column densities in the northern part of the M 82 outflow can be associated with cold disk gas detected in maps of HI and CO(l~O). We derive an Xeo factor which is somewhat lower as compared to that in our Galaxy. This is in good agreement with multi-transition line studies of various molecules in the disk of M82.

show abstract

Section: Xeo Determination In M 82supporting

confidence: 81%

The M82 Outflow: X-rays as a Probe for Neutral Disk Gas

Ott

Walter²,

Kerp³

2004

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

show abstract

“…• , with the southern side being more distant as for instance suggested by the higher reddening and polarization (Visvanathan & Sandage 1972;Notni & Bronkalla 1983;Chesterman & Pallister 1980), the motion of ionized gas (Götz et al 1990), and the geometry of the minor axis outflow (McKeith et al 1995;Shopbell & Bland-Hawthorn 1998). However, from an observed increase towards the north of free-free absorption due to ionized gas, Wills et al (2000) discuss the possibility of the opposite orientation.…”

Section: Orientation Of the Barmentioning

confidence: 98%

M 82's stellar bar

Greve

Wills

Neininger

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. The fueling of the starburst in M 82 may be related to a stellar bar which pushes gas towards the center where it forms stars. The observation by McKeith et al. (1993) of the near-IR Ca II photospheric absorption line allows a direct velocity measurement of the stars in M 82, and provides by this a confirmation of the predicted x1 and x2-orbits of the bar in M 82. From this and other observations we find that the mass of the x2-orbit stars is ∼15% of the mass of the bar, and that the mass of the bar of 2 × 10 9 M is 20-40% of M 82's mass. This mass concentration of ∼1 kpc extent at the center of M 82 underlines the dynamic importance of the bar.

show abstract

“…The minimum extinction implied by the proposed interpretation, Ev-1 = 0.5 mag, transforms to a face-on extinction in the plane, Av = 0.42 mag, similar to the value in our and other normal galaxies (reddening 0.5. cos78' = 0.17 mag; i M 78' for the outer disk, Notni and Bronkalla (1983)). …”

Section: Extinctionmentioning

confidence: 99%

Young stars in the disk of M82

1996

Self Cite

View full text Add to dashboard Cite

We present CCD V l c photometry in a field 1.9 x 1 . 3 square arcmin and positioned about 3 arcmin north-east of the centre of M82. More than 100 stars have been identified and measured above the photometric limits V = 23m5, I = 22m. Most of the objects fainter than V Starlike as well as 2-3 somewhat diffuse objects -candidates of globular clusters -preferentially occupy yellow colours in the colour-magnitude diagram; extreme blue and red objects are missing. The colour-magnitude diagram indicates continuing star formation in this part of the disk. The absence of blue stars is caused by reddening; no convincing explanation is found for the missing red supergiants. Young stars are distributed throughout the whole field, the youngest being concentrated in associations at the SW edge of the field. To cope with the very irregular background created by the galaxy's main body and with the low contrast of many of the stars against this background, a modified photometric method is introduced in which the background is estimated using the intensities in a ring drawn very tightly around the star in the wings of the point spread function.Key words: interacting galaxies -young stars -M82 A A A subject classification: 158 20" should be members of M82 as expected from the statistics of foreground stars. IntroductionThe galaxy M82, a member of the M81 group of galaxies, has been a favourite object to observers ever since Lynds and Sandage (1963) found evidence of energetic events in its central region, now known to be the seat of a huge starburst. Despite the vigorous starforming activity at its centre, the outer parts of M82 seem to show no sign of recent star formation; no HI1 regions, no bright young objects, and no spiral arms are seen. This led Sandage and Brucato (1979) to include it as a member of the small morphological group of "Amorphous Galaxies" showing no structure in their main body. The whole central M81 group is embedded in a huge cloud of intergalactic HI. It is now generally agreed that this cloud is the result of a passage of one or two galaxies (M82, NGC3077) near M81, leading to tidal disturbances especially in the interstellar medium of these galaxies. Tidal tails of HI are now seen joining the three galaxies (Appleton et al. 1981, Yun et al. 1994. The time passed since these events has been estimated by numerical modelling of the interaction; for M82 values between. 2...5 . lo8 yr have been found (for instance Kilian 1980, Brouillet et al. 1991).It has been suggested already by O'Connell and Mangano (1978) that the absence of young stars in the outer parts of M82 may be the result of this interaction, which severely disturbed the interstellar medium in M82, making further star formation impossible. Scattered star formation occured, however, in some limited regions in the disk, probably triggered by interaction with backfalling intergalactic material. If this scenario applies, the age 16 Astron. Nachr. 317 (1996) 4 226 Astron. Nachr. 317 (1996) 4 and the distribution of the youngest stars in the outskir...

show abstract

M82 — Tilt and Warp of its Principal Plane

Cited by 8 publications

References 6 publications

The M82 Outflow: X-rays as a Probe for Neutral Disk Gas

The M82 Outflow: X-rays as a Probe for Neutral Disk Gas

M 82's stellar bar

Young stars in the disk of M82

Contact Info

Product

Resources

About