1 / 18

Magnetic fields in perturbed galaxies: a sensitive measure of external influences or

Some terminology: Regular magnetic field: a unidirectional one: RM 0 Pseudo-regular field: an anisotropic random one: <Bx 2 > > <By 2 > RM=0.

malina
Download Presentation

Magnetic fields in perturbed galaxies: a sensitive measure of external influences or

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Some terminology: Regular magnetic field: a unidirectional one: RM0 Pseudo-regular field: an anisotropic random one: <Bx2> > <By2> RM=0 • Magnetic fields in perturbed galaxies: a sensitive measure of external influences • or • Why to observe abnormal galaxies when we don’t yet fully understand normal ones?

  2. 15% 10% 40% 1% NGC 4038/39 4.85 GHz DSS+TP+B-vec A merging pair Fundamental work by Chyży & Beck 2004,

  3. NGC 4038/39 4.85 GHz DSS+TP+B-vec A merging pair Fundamental work by Chyży & Beck 2004, Highly polarized „collisionregion” Low-polarization hidden SF region Highly polarized, steep spectrum outflow region

  4. a magnetic bridge? TP conts + PI B-vecs Drzazga, Chyży in prep. NGC 877

  5. NGC4490/85 another interacting pair Knapik et. al. in prep. Late type, no AGN

  6. NGC 4490/85 a magnetized stream?? HI image: Clemens, Alexander, Green 1998

  7. PV along this line and analogous along the NW arm Soida et al. 2001`

  8. NW normal region Diffuse CO(1-0) gas IRAM dish (Reuter et al. 1996) Clumpy CO(1-0) gas OVRO interf. (Soida et al. in prep) SE abnormal region Diifuse CO gas Clumpy CO gas

  9. Colour – clumpy cool gas seen by OVRO, conts – IRAM 1-0 upper panel: polarized intensity Colour – clumpy cool gas seen by OVRO, conts – HHT 3-2 upper panel: polarized intensity Data: OVRO –M. Soida, IRAM – Reuter et al. 1006 CO(3-2) HHT – Krakow + Bonn (M. Dumke, M. Krause, R. Wielebinski), in prep. A very personal remark: Without polarization observations probably these anomalies would remain unnoticed? Soida et al. in prep.

  10. Stephan’s Quintet IR – Appleton et al. Spitzer gallery X-rays – Trinchieri et al.. 2003

  11. Bt = 7G Bu = 1.5 G Bt = 8G Bu = 2G Soida et al. in prep. Genuine intergalactic (quasi) regular magnetic field TP conts+PI B-vecs VLA 6cm

  12. 15% 85% Motion? NGC 4501 in the Virgo Cluster TP+PI B-vecs, VLA 6cm Vollmer et al. 2007 + Kraków+Bonn& NRAO teams

  13. NGC 4501 rectified: Assymmetry of the magnetic pitch angles Data from Vollmer et al. 2007 + Kraków+Bonn & NRAO teams

  14. Polarization used to constrain the model Vollmer et al. (incl. Krakow, Bonn &NRAO teams) 2008 Pmax=2000cm-3(km s-1)2 twind= 80Myr

  15. Colour - HI ???? NGC 4654 TP contours +PI vecs VLA 20cm Radio data Vollmer et al. 2007 (incl. Krakow, Bonn & NRAO teams) HI Phookun & Mundy 1995.

  16. NGC 4535 – in southern Virgo extension – a „no reason” face-on case Vollmer et al. (incl. Krakow, Bonn & NRAO teams) 2007 Galaxy motion? NGC 4402 blown from the bottom? TP conts + PI vecs VLA 6cm Edge-on „no reason” case

  17. Motion? M86 environment NGC 4438 H (red) Kenney et al. 2008 X-rays (green) M. Weżgowiec from archive NEWTON-XMM data

  18. Attempt to summarize • We have observed: • Magnetic bridges • Anomalous arms • Compressional ridges • Magnetized outflows • Intergalactic magnetic fields Magnetic field as seen in polarization is a very good „preselector” of anomalies to be studied in detail in other domains (X-rays, HI dynamics etc.)

More Related