Coronal galaxy
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by
Budgieye
moderator
anyone want to do a discussion of this?
{EDIT: I don't know what a coronal galaxy is either]
Posted
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Ghost_Sheep_SWR
in response to Budgieye's comment.
Well sure, since it is interesting enough and I don't know what a 'coronal galaxy' is.
And, as I mentioned in the comments, this is a strange thing with an ionized OIII inner ring. The nucleus has (two?) cones that ionize the ring, but because the ring is rotating the effect is rather consistent around the whole ring.
On further thought might this be used to determine the past activity of the nucleus just as with Voorwerpjes? Because some parts are being ionized right now while other parts should be fading because they were ionized in the past.
Perhaps could be added to the sources used for AGN archeology? EDIT Would work like a clock actually đ
Posted
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bluemagi
http://www.solstation.com/x-objects/chimney.htm
I think this is what your looking for but am not sure. I never heard of a Coronal Galaxy. But I know it has hot ionized gaseous in Galactic Halo. Cheers,bluemagiPosted
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bluemagi
https://hologramuniverse.wordpress.com/2012/09/26/milky-way-galaxy-is-embedded-immersed-swimming-in-a-1-to-2-5-million-degree-plasma-gas-cloud-coronal-bubble/
Thought I'd add this one.BluemagiPosted
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Budgieye
moderator
Simple animation from NASA showing how beams of light from quasar illuminate galaxy Markarian 573. Nobody could explain it better. They don't call it a coronal galaxy so I wonder if this term is real.
Black Hole Sculpts an Hourglass Galaxy https://nasa.tumblr.com/post/165580689674/black-hole-sculpts-an-hourglass-galaxy
https://talk.galaxyzoo.org/#/subjects/AGZ0004nmm UGC_01214 #Seyfert2 #MRK_0573.
Jetlike Features in 4 galaxies by Alpha_Aurigae https://talk.galaxyzoo.org/#/boards/BGZ0000004/discussions/DGZ0000zw8
similar galaxy mention by Ghost_Sheep_SWR NGC 5252 + Voorwerp [OIII] images NGC 5252 + Voorwerp [OIII] images https://talk.galaxyzoo.org/#/boards/BGZ0000001/discussions/DGZ0002ksb
Hubble Space Telescope / NASA imagePosted
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bluemagi
Very interesting. So what is it called? Any of the scientists know? Thanks, bluemagi
Posted
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Budgieye
moderator
Coronal-Line Forest Active Galactic Nuclei? CLiF AGN . Recent references have a pay barrier so I can't read them. eg http://adsabs.harvard.edu/cgi-bin/bib_query?2015MNRAS.451L..11R
EDIT:
https://en.wikipedia.org/wiki/Galactic_corona
Corona apparently is used to describe a hot area in our own Milky Way, but is now starting to be used when describing other galaxies?
Posted
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bluemagi
https://www.oa-roma.inaf.it/GVBH/Program_files/jwang_sicily.pdf
Budgieye I think I found something. Maybe its better if I don't know what its called I seem to find it. They seem to call it a nuclear outflow, thats all in the way of a name. Thanks,bluemagiPosted
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Budgieye
moderator
Good find with nice pictures..... I like pictures. EDIT I see there is a montage by Galaxy Zoo B. Keel.
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bluemagi
Budgieye. If you need more let me know. The professor I worked for, used to call me tenacious at research. Thanks, bluemagi
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How about this for timing?
https://www.nasa.gov/image-feature/goddard/2017/hubbles-cool-galaxy-with-a-hot-corona
Ps. Is this galaxy (UGC 1214) yet used for archeological AGN studies or not?
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Budgieye
moderator
Here is a picture of the X-ray corona.
HOT X-RAY CORONAE AROUND MASSIVE SPIRAL GALAXIES: A UNIQUE PROBE OF STRUCTURE FORMATION MODELS
http://iopscience.iop.org/article/10.1088/0004-637X/772/2/97/meta
- INTRODUCTION
The presence of hot gaseous coronae in dark matter halos of massive galaxies is a fundamental prediction of structure formation models (White & Rees 1978). This gas collapse scenario in a cold-dark-matter-dominated universe was applied by White & Rees (1991), who predicted that dark matter halosâsurrounding all types of present epoch massive galaxiesâshould have an associated X-ray luminous corona.
X-ray luminous, hot gaseous coronae are nearly ubiquitous for massive early-type galaxies. First discovered with the Einstein Observatory (Forman et al. 1985), these coronae have been extensively studied (e.g., Sarazin et al. 2001; Jones et al. 2002; Mathews & Brighenti 2003; BogdĂĄn & Gilfanov 2011). Early-type galaxies exhibit at least three X-ray emitting components. (1) A well-studied population of low-mass X-ray binaries (LMXBs), which add a notable contribution to the total X-ray emission of galaxies (Gilfanov 2004; Zhang et al. 2012); (2) emission from active binaries (ABs) and cataclysmic variables (CVs), whose total emission is proportional to the stellar mass of the galaxy (e.g., Revnivtsev et al. 2008; BogdĂĄn & Gilfanov 2011), and (3) thermal, sub-keV gas, produced from the galaxy's own constituent stars or from infall of group/cluster gas in central bright cluster galaxies. For massive early-type galaxies, it is difficult to detect the more extended atmospheres of hot gas, since they either have bright coronae from stellar mass loss and/or lie in larger dark matter halosâgroups and clustersâthat have their own gaseous atmospheres. Thus, elliptical galaxies are not suitable for probing the luminous X-ray gas predicted around individual galaxies.
However, late-type, spiral galaxies also are predicted to have luminous X-ray coronae and can test galaxy formation scenarios (White & Rees 1991). A major advantage of spirals is their location, whereas massive ellipticals lie either in the center of galaxy groups and clusters and/or in rich environments, it is possible to find relatively isolated and quiescent massive spiral galaxies. Starburst galaxies or galaxies undergoing mergers are not suitable to characterize the extraplanar X-ray emission. Due to UV, far-infrared, and Hα imaging, large star formation rates (SFRs), and hence starburst galaxies, can be identified, and merging galaxies can be recognized based on their optical appearance. Thus, isolated massive spiral galaxies with moderately low SFRs and relatively undisturbed morphology are the ideal targets for exploring the extraplanar X-ray coronae, thereby testing structure formation models.
The observed X-ray emission from spiral galaxies consists of multiple components: (1) in addition to LMXBs (Gilfanov 2004), bright high-mass X-ray binaries, associated with star formation, are located in the star-forming regions (Grimm et al. 2003); (2) an additional important contributor to the X-ray flux is the collective emission of faint compact X-ray sources, which contribute to the unresolved, diffuse component. The population of ABs and CVs follow the stellar light distribution (Revnivtsev et al. 2008), while the emission from young stars and young stellar objects is proportional with the SFRs of the host galaxy (BogdĂĄn & Gilfanov 2011). (3) Additionally, spiral galaxies host at least moderate amounts of ionized gas with sub-keV temperatures (BogdĂĄn & Gilfanov 2011). These components, enumerated above, provide the bulk of the observed emission within the optical extent of spiral galaxies and are very difficult to model accurately as an integrated component to detect the faint outer corona projected onto this complex region. Therefore, to probe the structure formation models, the hot X-ray coronae must be explored beyond the optical extent of spiral galaxies.
The primary goals of the present paper are twofold. First, we aim to detect and characterize the hot X-ray coronae beyond the optical disks of two massive spiral galaxies, NGC 1961 and NGC 6753, based on moderately deep XMM-Newton X-ray observations. Second, we aim to confront the observed physical properties of the X-ray coronae with those predicted by modern structure formation models.
Posted
- INTRODUCTION